# Stars/Star fissions

(Redirected from Star fission)
W Ursae Majoris is an eclipsing binary, specifically a contact binary with a common envelope. The primary component has a radius of 1.08 solar. The secondary has a 0.78 solar radius. Credit: Aladin at SIMBAD.

Star fission is the splitting of a star at a critical angular momentum, or period in its history, with the consequence of zero-age contact in the resultant binary star. This splitting may have its highest probability of occurring during early star formation.

## Stars

This image shows the star Merope (23 Tauri) in the Pleiades. Credit: Henryk Kowalewski.

Def.

1. any small luminous dot appearing in the cloudless portion of the night sky, especially with a fixed location relative to other such dots or
2. a luminous celestial body, made up of plasma (particularly hydrogen and helium) and having a spherical shape

is called a star.

## Stellar astronomy

When any effort to acquire a system of laws or knowledge focusing on a stellar astr, aster, or astro, that is, any natural star in the sky especially at night, succeeds even in its smallest measurement, stellar astronomy is the name of the effort and the result.

## Stellar astrophysics

This plot gives an example of the mass-luminosity relationship for zero-age main-sequence stars. The mass and luminosity are relative to the present-day Sun. Credit: RJHall.

Def. "any object forming on a dynamical timescale, by gravitational instability", is called a star.[1]

Instantaneous zero-age star formation is defined by the 0 Myr grids of the H II region emission line spectrum, specifically the ionizing spectral energy distribution (normalized to the flux at the Lyman limit).[2]

Stars along the main sequence fall into zero-age mass ranges:[3]

• Stars below about 8 Mʘ (solar mass) do not explode as supernovae. This is obviously most stars;
• Stars from about 8 to about 15 Mʘ explode as supernovae, but do not have a strong stellar wind, and so explode into the interstellar medium;
• Stars from about 15 to 25 Mʘ have a substantial wind; the wind is enriched only in helium, where the chemical composition of the wind at the time of explosion is approximately 0.5 in He and 0.5 in H. The mass in the shell of wind-swept material is moderate;
• Stars from about 25 Mʘ have a strong wind, enriched in heavy elements with little hydrogen left. The mass in the shell of wind-swept material is large.

The ‘zero-age’ for a star is when it first appears on the Hertzsprung-Russell diagram by burning hydrogen in its core through nuclear fusion reactions.[4]

## Planetary sciences

"The deficiency of some noble metals in the crust of the earth has been explained for many years as the result of leaching by a metallic phase (chiefly iron) which later formed the earth's core."[5]

"A broadly similar deficiency also exists in the moon; but the moon has almost no core."[5]

If "the moon was formed by fission of the earth (followed by intense volatilization) after the core of the earth had formed [...], then the earth must have existed for some time as a liquid mass, before dividing."[5]

"A Maclaurin ellipsoid rotating near the upper limit of dynamical stability is, in principle, secularly unstable with respect to a transformation to a triaxial, Jacobi ellipsoid."[5]

For "a loss of mechnical energy (by conversion to heat); [the transformation] will therefore proceed very slowly if the ellipsoid has low viscosity. Thus the core can form while the viscosity is low, and eventually, falling temperature and rising viscosity will result in fission, by way of an unstable Jacobi ellipsoid."[5]

## Colors

"The ancient and massive Koronis family now has four identified subfamilies (asteroid families made by the breakup of fragments of the ancient collision), with ages running from 5.7 to 290 My."[6]

"Analysis of family members with accurate SDSS measurements shows a correlation of average subfamily color with age [...] The reddening trend with age remains even when comparing only asteroids of similar size, confirming the presence of space weathering phenomena."[6]

The origin of the "bluer colors of small objects:

1. those objects receive more jolts from random collisions capable of shaking the regolith and exposing fresh material beneath;
2. those objects receive more jolts from the cycle of fission and recombination driven by YORP; and
3. the lower gravity on those objects retains regolith less well."[6]

"Since all families in Figure 2 are made from the same original material, we interpret the differences between them in terms of processes over time. The mechanism that caused the break in the old Koronis data, began after 6 My and was complete by 220 My (though the reddening continued beyond 220 My)."[6]

"YORP torques lead many objects to fission and then reaccrete. The reaccretion event may be energetic enough to freshen the regolith. This effect works better for smaller objects as needed [Or,] proportionate collisions could have outcomes that differ with size due to varying surface gravity. It is easier to knock the weathered regolith clear of the asteroid altogether for small asteroids."[6]

## Minerals

"Piezonuclear reactions, which occur in inert and non-radioactive elements, are induced by high pressure and, in particular, by brittle fracture phenomena in solids under compression. These low-energy reactions generally take place in nuclei with an atomic weight that is lower or equal to that of iron (Fe)."[7]

Pressure, "exerted on radioactive or inert media, can generate nuclear reactions and reproducible neutron emissions. In particular, low-energy nuclear reactions and heat generation have been verified in pressurised deuterium gas [...] and in radioactive deuterium-containing liquids during ultrasound and cavitation".[7]

"Neutron emission measurements, by means of helium-3 neutron detectors, occurred during crushing failure [...] in particular regard neutron emissions from granite (gneiss) specimens [...] transforming heavier (Fe) into lighter (Mg, Al, Si) atoms."[7]

The "neutron measurements obtained from two granite specimens under compressive loading condition have exceeded the neutron background by approximately one order of magnitude, in correspondence to their brittle failure [...] for the fracture experiments on green Luserna Granite specimens [...], analysis of the fracture surfaces, conducted by energy dispersive X-ray spectroscopy, has shown a considerable reduction in the iron content (25%) [...] This iron decrease is counterbalance by an increase in aluminium, silicon, and magnesium. In particular, the increase in aluminium content corresponds to the 85% of the iron decrease. Therefore, the piezonuclear fission reactions [are]:"[7]

${\displaystyle Fe_{26}^{56}\rightarrow 2Al_{13}^{27}+2neutrons}$
${\displaystyle Fe_{26}^{56}\rightarrow Mg_{12}^{24}+Si_{14}^{28}+4neutrons.}$

Granite "is predominantly constituted by quartz and feldspar minerals"."[7]

"Neutron emissions measured near the Earth's surface exceeded the neutron background by about one order of magnitude in correspondence with seismic activity and more appreciable earthquakes [...] This relationship between the processes in the Earth's crust and neutron flux variations has allowed increasing tectonic activity to be detected and methods for short-term prediction and monitoring of earthquakes to be developed"."[7]

Additional "piezonuclear fission reactions that could take place in correspondence with plate collision and subduction:"[7]

${\displaystyle Co_{27}^{59}\rightarrow Al_{13}^{27}+Si_{14}^{28}+4neutrons,}$
${\displaystyle Ni_{28}^{59}\rightarrow 2Si_{14}^{28}+3neutrons,and}$
${\displaystyle Ni_{28}^{59}\rightarrow Na_{11}^{23}+Cl_{17}^{35}+1neutron.}$

## Theoretical stellar astrophysics

The "star formation process happens very quickly and in regions of the Galaxy that are difficult to study observationally."[8]

## Theoretical star fissions

Nonaxisymmetric "magnetic instabilities can be readily produced from a toroidal magnetic field [...] in rotating spherical systems. [As can] the growth rate of the three-dimensional magnetic instabilities. [Magnetic] field and velocity perturbations with small radial and latitudinal scales can effectively extract energy from the basic toroidal field and grow. [The] most unstable mode of the instabilities is always three-dimensional and characterized by small radial and latitudinal scales."[9]

A deep "strong toroidal magnetic field suppresses turbulent convection and dramatically reduces the α-effect [...] Other dynamo processes must replace the conventional turbulent dynamo in this situation."[9]

In "an interface dynamo [...] turbulent convective motions in an upper region produce an α-effect generating a weak magnetic field that penetrates into the neighboring lower region."[9]

## Binary stars

Def. two stars that appear to be one when seen with the naked eye, either because they orbit one another (binary stars) or happen to be in the same line of sight even though they are separated by a great distance is called a double star.

Def. a star that appears as a double due to an optical illusion; in reality, the stars may be far apart from each other is called an optical double.

Def. two stars which form a stellar system, such that they orbit the point of equilibrium of their gravitational fields is called a double star.

Def. a stellar system that has two stars orbiting around each other is called a binary star.

A binary star is a star system consisting of two stars orbiting around their common center of mass. The brighter star is called the primary and the other is its companion star, ... or secondary. Many visual binaries have long orbital periods of several centuries or millennia and therefore have orbits which are uncertain or poorly known.

Def. a binary star whose components can be visually resolved is called a visual binary.

"The overall frequency of occurrence of binary stars among the [pre-main sequence] PMS population is at least as large as has been documented for main-sequence stars (Duquennoy & Mayor 1991), that is, certainly greater than 50%."[8]

"Young, stellar-mass binary systems have been found with semimajor axes ranging from 0.02 to 103 AU (orbital periods ranging from a couple of days to 104 years), with a binary frequency distribution as a function of semimajor axis that is qualitatively consistent with the log-normal–like distribution found for main-sequence stars. With this evidence in hand, Mathieu (1994) concluded that “binary formation is the primary branch of the star-formation process.”"[8]

## Contact binaries

A contact binary is a binary star system whose component stars are so close that they touch each other or have merged to share their gaseous envelopes. ... Almost all known contact binary systems are eclipsing binaries;[10] eclipsing contact binaries are known as W Ursae Majoris variables, after their type star, W Ursae Majoris.[11]

## Zero-age contacts

“Zero-age contact must be a consequence of star fission under critical angular momentum.”[12] When the angular momentum is too large, the star breaks into a detached binary.[12] When the angular momentum is too small, the star remains as a single star.[12] BH Centauri and V1010 Ophiuchi have zero-age radii and are zero-age contact systems.[12] BH Centauri is an overcontact system.[12]

## Common envelope binaries

This diagram suggests a reverse common envelope process for binary star formation. Credit: Marshallsumter and Cryptic C62 *derivative work: Trex2001.

[A] common envelope (CE) refers to a short-lived (months to years) phase in the evolution of a binary star in which the largest of the two stars (the donor star) has initiated unstable mass transfer to its companion star. Breach of the common envelope crosses the Lagrange Point L1 with the donor-star mass beyond the Roche Lobe acting as the third dynamic point in a formerly binary system. Mass transfer is unstable when the radius of the donor star expands more rapidly or shrinks less rapidly than does the binary orbit. Hence, the donor will start mass transfer when it overfills its Roche lobe and as a consequence the orbit may shrink while the star expands, causing it to overflow the Roche lobe even more, which accerelates the mass transfer, causing the orbit to shrink faster and the donor to expand faster, etcetera. This leads to the run-away process of dynamically unstable mass transfer. The result will be the fast expansion of the donor's stellar envelope, which will then engulf the companion star. Hence the name common envelope.

The diagram on the right suggests a reverse common envelope process for binary star formation. At some point in star formation, two cores, one for a main-sequence star (yellow) and the other for a red giant (gray) form within a common envelope. As mass transfer continues or decelerates, the red giant transfers to at or below its Roche lobe (dashed black line) and a partially stable binary is formed.

## Overcontact systems

This is a computer generated picture of V701 Scorpii. Credit: K.-C. Leung and Robert E. Wilson.

When stars share an envelope the pair may be called an overcontact binary.[13][14][15]

BH Centauri is a zero-age overcontact binary system with primary and secondary masses equal to (9.4±5.4) and (7.9±5.4) Mʘ.[16] With later analysis including more recent data, "the mass ratio went from 0.97 to 0.84, and the degree of overcontact went from 21% to 48%."[16]

V1010 Ophiuchi and V701 Scorpii are both overcontact systems.[17] For V1010 Ophiuchi "the masses are 2 and 1 M while the radii are 2.1 and 1.5 R. The location in the HR diagram suggests that they are zero-age stars, as do the radii".[17]

At the right is a computer generated picture of the overcontact system V701 Scorpii. The overcontact in V701 Scorpii appears to be almost twice as much as in V1010 Ophiuchi.

"Most people would agree that fission is the most probable way to form binary systems, especially the close systems. The angular momentum must be the deciding factor as to whether a gas cloud becomes a single star or a binary system."[17]

## Dynamos

"[M]otions resulting from [a linear magnetohydrodynamic] instability act as a dynamo to sustain the magnetic field."[18] "Supersonic flows are initially generated by the Balbus-Hawley magnetic shear instability."[18]

A plasma with local magnetohydrodynamic instabilities creates mechanical turbulence, motion, or shear (a dynamo) which in turn generates or sustains the local magnetic field.

When this magnetohydrodynamic dynamo occurs between or within radiative layers, a radiative dynamo is operating.

There are three requisites for a dynamo to occur and subsequently operate:

• An electrically conductive fluid medium such as a plasma or liquid iron
• local magnetohydrodynamic instabilities
• An energy source to create the local magnetohydrodynamic instabilities and to drive mechanical turbulence, motion, or shear within the fluid.

Def. any conversion of mechanical energy into electrical energy and associated magnetic fields is called a dynamo.

Def. "a dynamo taking place in the radiative layers"[19] of a star, or other astronomical object, is called a radiative dynamo, or stellar radiative dynamo.

## Interstellar magnetic fields

The "interstellar magnetic field significantly influences the onset of gravitational collapse in molecular clouds, the general consensus is that the field will largely decouple from a contracting cloud at number densities ≳1010 cm−3 because, at such high densities, the fractional ionization of the gas becomes extraordinarily small."[8]

The "processes likely to be responsible for transforming single gas clouds into binary protostellar systems largely operate at densities higher than this limit".[8]

## Binary star formations

Binary and multi-star systems consist of two or more stars that are gravitationally bound, and generally move around each other in stable orbits. When two such stars have a relatively close orbit, their gravitational interaction can have a significant impact on their evolution.[20] The masses of stars are determined from computation of the orbital elements.

Large lengths, such as the radius of a giant star or the semi-major axis of a binary star system, are often expressed in terms of the astronomical unit (AU)—approximately the mean distance between the Earth and the Sun (150 million km or 93 million miles).

The most common multi-star system is a binary star, but systems of three or more stars are also found. For reasons of orbital stability, such multi-star systems are often organized into hierarchical sets of co-orbiting binary stars.[21] Larger groups called star clusters also exist. These range from loose stellar associations with only a few stars, up to enormous globular clusters with hundreds of thousands of stars.

If components in binary star systems are close enough they can gravitationally distort their mutual outer stellar atmospheres. In some cases, these close binary systems can exchange mass, which may bring their evolution to stages that single stars cannot attain. Examples of binaries are Sirius and Cygnus X-1 (of which one member is probably a black hole). Binary stars are also common as the nuclei of many planetary nebulae, and are the progenitors of both novae and type Ia supernovae.

The observation of binaries consisting of pre-main sequence stars, supports the theory that binaries are already formed during star formation.

"The question of binary star formation is now regarded as a central unsolved issue in star formation, given the observational evidence that the majority of stars are in binary systems both during the main sequence ... and pre-main sequence stages".[22] "[T]he 'theory gap' currently separating theoretical models from the observations they purport to describe is the major unsolved problem in this area."[22]

## Bifurcations

Def. a division into two is called bifurcation.

Bifurcation means the splitting of a main body into two parts. Bifurcation theory is the study of bifurcation in dynamical systems.. The forking of a river into its tributaries is referred to as river bifurcation. A bifurcation can be a false dilemma in which two alternative statements are held to be the only possible options when there are more options. In cybernetics, a bifurcation is when a system switches from one stable state to another, where minor fluctuations may play a crucial role in deciding the outcome.

“About a century ago, Liapounov and Poincaré found that the sequence of Jacobi’s ellipsoids branches towards pear-shaped configurations for sufficiently high rotation.”[23]

Equatorial break-up and instability occur at the point of bifurcation.[24]

“Bifurcation of protostars can occur because of excessive angular momentum either during hydrodynamic collapse (‘fragmentation’), or else after the star has arrived on the HR diagram as a visible, slowly contracting star (‘fission’).”[25]

Spectral types B2-B5 and F3-G2 binaries with orbital periods shorter than 10 or 100 yr may result from the bifurcation of rapidly rotating protostars.[26]

Binary formation by ... bifurcation is difficult to achieve theoretically for compressible viscous gases and may not occur frequently or ever.[27]

Systems of spectroscopic binaries of periods less than 3.6 days "involve separations that are less than 2.5 times the sum of the radii of the components."[27]

These systems "probably have already exchanged mass and no longer have their original mass ratios."[27]

For these systems, we are unable to give their mecahnisms of origin.[27]

Provisionally, "most or all binaries [are] formed in capture processes (including initial star formation in bound systems) and that bifurcation or fission need not have occurred frequently."[27]

For the inclusion of compressibility and viscosity in theoretical calculations, "it is very difficult to produce binaries by fission and only under special circumstances."[27]

“In view of the high frequency of spectroscopic binaries, the formation mechanism must be a frequent one, not a rare occurrence."[27]

For most binaries to result from fission of a star into at least two stars, the expanding separation between the binaries must result in capture rather than expulsion from the system.

## Fissions

In the first frame, a neutron is about to be captured by the nucleus of a U-235 atom. In the second frame, the neutron has been absorbed and briefly turned the nucleus into a highly excited U-236 atom. In the third frame, the U-236 atom has fissioned, resulting in two fission fragments (Ba-141 and Kr-92) and three neutrons, all with large amounts of kinetic energy. Credit: Fastfission.

Def. the process of splitting into smaller particles is called fission.

"Binary formation by fission or bifurcation of a contracting rotating protostar" is difficult to achieve theoretically for compressible viscous gases and may not occur frequently or ever.[27]

Generally, fission is the splitting of something into two parts. In anthropology, fission is the process whereby a nation-state divides and becomes multiple states. In biology, fission is the subdivision of a cell or a multi-cellular body into two or more parts and the regeneration of each of the parts into a complete individual. In physics, nuclear fission is a nuclear reaction in which an atomic nucleus "splits into smaller parts (lighter nuclei), often producing free neutrons and photons (in the form of gamma rays), and releasing a tremendous amount of energy A large atomic nucleus such as uranium (236U) is split into two smaller particles (141Ba and 92Kr). Most nuclear fissions are binary fissions, but occasionally (2 to 4 times per 1000 events), three positively-charged fragments are produced in a ternary fission.

"Most people would agree that fission is the most probable way to form binary systems, especially the close systems."[17]

"[F]ission is now commonly considered to be the most likely explanation for the existence of close binaries".[28] But, "the hypothesis cannot be regarded as proved until the evolution of a rotating protostar has been followed from an initial state as a single star to a final state as a detached binary system."[28] "[T]he high frequency of close binaries over a wide mass range surely implies that no special characteristics of the properties of stellar matter are essential to binary formation".[28] "[T]he initial departure from axial symmetry is due to the onset of dynamical overstability for a mode of low order".[28] "[G]ravitational torques between the debris and the main component (i.e., before fission) significantly influence the latter’s evolution."[28] "[G]eneral trends emerge ... :

1. [f]ollowing the appearance of departures from axial symmetry, a substantial fraction of mass is nearly always lost as debris,
2. [e]volution into a bar-shaped structure is common ... ,
3. [when] fission [occurs], it leads to a binary of small mass ratio, typically towards the lower end of the range 0.1-0.5."[28]

With "significant mass exchange ... during [the] contact phase ... , the mass ratio immediately following fission may have little relevance to observed mass ratios."[28]

"[F]ission [can] occur only in stars whose interior state at least approximates to incompressibility. With even the lowest degree of central condensation which [may] occur in a purely gaseous star, fission [is] an impossibility, [as] any excess of angular momentum [relieves] itself by equatorial ejection of matter" as debris.[29] "About one-third of the stars observed ... are binaries which have almost certainly been formed by fission, so that these, at least, must have been in something approximating to the liquid [or fluid] state when fission took place."[29] "At different temperatures the atoms [are] of different sizes through being ionized down to different levels."[29]

"The idea of fission in rapidly rotating stars [is] not a return to the classical fission theory of Darwin and Jeans."[30] “If fission occurs at all, it is probably catastrophic in character and has little resemblance to rotational breakup.”[30] "[M]any close binaries are now in effect single objects possessing two massive nuclei, and a single envelope surrounding them."[30] When such as object "tends to shed its envelope, exposing the separate nuclei as a normal double star, we [shall] call this process fission."[30] When "the trend is in the opposite direction, we should probably speak of fusion."[30]

## Fragmentations

Def.

1. a part broken off
2. a small, detached portion
3. an imperfect part

is called a fragment.

Def. the act or process of producing a fragment is called fragmentation.

Fragmentation of the molecular cloud during the formation of protostars is an acceptable explanation for the formation of a binary or multiple star system.[31][32]

With respect to low-mass star formation, "fragmentation to form a binary star [may be] most simply achieved if collapse is initiated by an external impulse."[33] "On its own, [the] process under which a dense molecular cloud core can collapse to form a binary, or multiple, star system would produce wide binaries".[33] "[C]lose binaries [may be] formed because of mutual interactions between the protostellar discs surrounding the various fragments."[33] "[T]he most likely collision which has an effect on the core is the one for which [the velocity change imparted by the impulse,] Δv ~ cs [(the internal sound speed),] induced by a clump of mass ~0.1M."[33] "[T]he impulsive collapse of the cloud cores [requires] that they are not primarily magnetically supported in their central regions."[33]

"The sources are separated by 17", or 4200 AU. Binary separations of this order are consistent with early fragmentation in a relatively dense cloud ("prompt initial fragmentation," e.g., Pringle 1989; Looney et al. 2000), in which case the individual sources would have distinct protostellar envelopes."[34]

"In a binary formed via gravitational fragmentation, we would expect the separation to correspond to the local Jeans length (Jeans 1928):"[34]

${\displaystyle \lambda _{J}=({\pi c_{s}^{2} \over G\mu _{p}m_{H}n})^{1/2},}$

"where cs is the local sound speed, and μp = 2.33 and n are the mean molecular weight and mean particle density, respectively. A Jeans length of 4200 AU would require a relatively high density (n ~ 6 x 105 cm−3, assuming cs = 0.2 km s−1). The mean density of the Per-Bolo 102 core, measured within an aperture of 104 AU, is 4 x 105 cm−3, close to the required value."[34]

## Fissions by fusions

A binary star system that includes a nearby white dwarf can produce certain types of spectacular stellar explosions, including the nova and a Type 1a supernova.[20] The explosion is created when the white dwarf accretes hydrogen from the companion star, building up mass until the hydrogen undergoes fusion.[35]

## Gravitational captures

While it is not impossible that some binaries might be created through gravitational capture between two single stars, given the very low likelihood of such an event (three objects are actually required, as conservation of energy rules out a single gravitating body capturing another) and the high number of binaries, this cannot be the primary formation process.

KIC 9832227 in 2013 " the speed of the orbit was gradually getting faster and faster, implying the stars are getting closer together. The pair is so close, in fact, they share an atmosphere [...] V1309 Scorpii, which also had a merged atmosphere, was spinning up faster and faster, and exploded unexpectedly in 2008."[36]

The "pair will explode as a “red nova”—an explosion caused by a binary merging—in about 5 years’ time."[36]

## Supernova remnants

This image shows X-ray observations by XMM-Newton in purple of supernova remnant SNR MSH 11-16A. Credit: NASA/CXC/UC Berkeley/J.Tomsick et al & ESA/XMM-Newton.
The image is a close-up of the small green object in the above image. Credit: NASA/CXC/UC Berkeley/J.Tomsick et al & ESA/XMM-Newton.

The image at right is an X-ray astronomy image of "the supernova remnant SNR MSH 11-16A, located about 30,000 light years away [in the constellation Carina]. The purple glow is [a coloration] from X-rays emitted by the gas superheated to millions of degrees by the explosion."[37]

The second image at right is an enlargement of the Chandra X-ray Observatory image (in green) of the first image. "The Chandra image reveals a comet-shaped X-ray source well outside the boundary of the supernova remnant. This source consists of a point-like object with a long tail trailing behind it for about 3 light years."[38]

"The point-like X-ray source was discovered by the International Gamma-Ray Astrophysics Laboratory, or INTEGRAL, and is called IGR J11014-6103 (or IGR J11014 for short). The elongated emission is pointing towards the center of MSH 11-61A where the pulsar would have been formed. Another interesting feature of the Chandra image, also seen with XMM-Newton, is the faint X-ray tail extending to the top-right. The cause of this feature is unknown, but similar tails have been seen from other pulsars that also do not line up with the pulsar's direction of motion."[38]

"Based on earlier observations, astronomers estimate that the age of MSH 11-61A, as it appears in the image, is approximately 15,000 years, and it lies at a distance of about 30,000 light years away from Earth. Combining these values with the distance that the pulsar has appeared to have traveled from the center of the MSH 11-61A, astronomers estimate that IGR J11014 is moving at a speed between 5.4 million and 6.5 million miles per hour."[38]

## Entities

"While many stars form in binary systems, binary formation is still not well understood. This is particularly true for close binary systems with orbital periods of a few days. If the orbital characteristics of these systems would not have changed since pre-main-sequence then the stars would have formed from one entity, as during the pre-main-sequence phase their sizes were bigger. As fission seems unlikely (Tohline 2002), the orbit probably shrunk and therefore the angular momentum of these systems must have undergone a complex history. One part of the angular momentum distribution which is seldom probed is the stellar spin."[39]

There are spin "aligned systems and [...] spinorbit misalignment. [Stellar] obliquity seems not to be a simple function of orbital distance or eccentricity."[39]

In "the DI Herculis system [...] rotation is strongly misaligned with the orbital spin".[39]

## Sources

Sources of stellar energy: "The potential energy of a nuclide is enhanced by about 10 MeV per nucleon from the repulsion between like nucleons and diminished by about 20 MeV per nucleon from the attraction between unlike nucleons."[40]

"Nuclear stability results mostly from the interplay of these opposing forces, plus Coulomb repulsion of positive charges. While fusion may be the primary mechanism by which first generation stars produce energy, repulsion between like nucleons may cause neutron emission from the collapsed core (neutron star) produced in a terminal supernova explosion and initiate luminosity in second generation stars that accrete on such objects."[40]

"… in the evolution of elements much more material has gone into the even-numbered elements than into those which are odd…”[41]

"In the 1920s, Payne [3] and Russell [4] reported that the Sun’s atmosphere consisted mostly of hydrogen (H) and helium (He), but Hoyle [5] notes that he and others "in the astronomical circles to which I was privy" (p. 153) continued until after the Second World War to believe that the Sun was made mostly of iron. Then Hoyle notes that "much to my surprise" (p. 154), the high-hydrogen, low-iron model was suddenly adopted without opposition."[40]

"Perhaps research on H-fusion for thermonuclear weapons lead scientists to revise their opinions about the interior of the Sun. Teller [6] reports that Gamow, Critchfield and Bethe had concluded that fusion reactions "… keep stars going" (p. 67) before the discovery of fission in December of 1938 and "We were all convinced … that we could accomplish a thermonuclear explosion" and this was "one of the laboratory’s objectives" (p. 70) when the Los Alamos Laboratory was established in 1943. The new weapon from Los Alamos in 1945 was based on a fission explosion that was later to provide the trigger for the hydrogen bomb."[40]

"Fusion has been widely believed to be the energy source for the Sun and other stars. Burbidge et al. [19] showed that elemental and isotopic abundances in the solar system could be understood in terms of reasonable nuclear reactions that might occur as a first generation star, consisting initially of hydrogen, underwent normal stages of stellar evolution up to and including its terminal explosion as a supernova (SN)."[40]

"If the Sun, a second generation star, formed on the collapsed SN core [...] then repulsion between neutrons could be the driving force for neutron emission from the collapsed core of the supernova that produced our elements. This may be the first, and the rate-determining, step in the production of solar luminosity and the Sun’s outward flow of solar-wind (SW) protons [15]:"[40]

1. Escape of neutrons from the collapsed SN core;
2. Decay of free neutrons or capture by other nuclides;
3. Fusion of most H+ during its upward migration, carrying lighter elements and the lighter isotopes of each element to the solar surface; and finally the
4. Annual escape of 3 x 1043 H+ in the solar wind.

## Neutrons

"The feasibility of thermal neutron fission and fast neutron fission in planetary and protostellar matter [may be] calculated from nuclear reactor theory. Means for concentrating actinide elements and for separating actinide elements from reactor poisons [exist]. [I]ntermittent or interrupted planetaryscale nuclear fission breeder reactors [may occur] in connection with observed changes in the giant outer planets and changes in the geomagnetic field. [T]hermonuclear fusion reactions in stars are ignited by nuclear fission energy [...] dark matter, inferred to exist in the Universe, might be accounted for, at least in part, by the presence of dark stars (not necessarily brown dwarfs) whose protostellar nuclear fission reactors failed to ignite thermonuclear fusion reactions."[42]

## Opticals

"For a few special cases, rotational velocities for protostars have been obtained directly from observations of the outer optically thin regions. In the case of B335, [...] Ω = 1.4 x 10-14 s-1, uniform out to a radius of 0.22 pc, from velocity gradients in 13CO and C18O. A univorm-density sphere of that radius would have j = 2.6 x 1021 cm2 s-1, consistent with the lower end of the observed range. Rotation is not important in determining the force balance in the outer regions, and [...] this object is in fact undergoing gravitational collapse."[43]

## Submillimeters

"Interferometry at 870 µm [...] has been used to resolve the compact inner dust disks in the sources HL Tau and L1551 IRS 5; the disk radii are 60 and 80 AU, respectively, and the disk planes are apparently perpendicular to the bipolar flows."[43]

Millimeter "interferometry [has been used] to infer the presence of a 45 AU disk in L1551 IRS 5."[43]

In "the system IRAS 16293 - 2422 [observations] at cm, mm and submillimeter wavelengths indicate that this source is a binary system, with a separation 800 AU and with two associated bipolar outflows. The orbitl j = 4.5 x 1020 cm2 s-1, assuming each component has a mass of 1 M. Surrounding the binary pair is a circumbinary disk with an outer radius of 2000 AU and projected rotational velocity of ≈ 0.75 km s-1. [...] the j at its outer edge can be estimated to be 2.25 x 1021 cm2 s-1. These angular momenta are quite consistent with those in the cores of molecular clouds; the binary could have fragmented out of the inner portions of the core (which have lower angular momentum than average), while the circumbinary disk could have formed from the outer regions. Thus this system [...] well illustrates the commonly accepted picture that the angular momenta of cloud cores are transformed during the collapse phase into the orbital motion of disks and binary systems."[43]

## Sun

Arcs rise above an active region on the surface of the Sun in this series of images taken by the STEREO (Behind) spacecraft. Credit: Images courtesy of the NASA STEREO Science Center.

Def. the star which the Earth revolves around and from which it receives light and warmth.[44] is called the sun.

Depending on context and the definition of a star, the sun may or may not be included.

The mass of the coronal ejection in the image at right is many times that of the Earth. As the Sun itself remains, the ejection may be a fragmentation.

## Mira

This is a real visual image of the red giant Mira by the Hubble Space Telescope. Credit: Margarita Karovska (Harvard-Smithsonian Center for Astrophysics) and NASA.
This is a NASA Hubble Space Telescope image of the cool red giant star Mira A (right) and its nearby hot companion (left) taken on December 11, 1995 in visible light. Credit: Margarita Karovska (Harvard-Smithsonian Center for Astrophysics) and NASA.

A red giant is a luminous giant star. The outer atmosphere is inflated and tenuous, making the radius immense and the surface temperature low, somewhere from 5,000 K and lower. The appearance of the red giant is from yellow orange to red, including the spectral types K and M, but also class S stars and most carbon stars. The most common red giants are the so-called red giant branch stars (RGB stars). Another case of red giants is the asymptotic giant branch stars (AGB). To the AGB stars belong the carbon stars of type C-N and late C-R. The stellar limb of a red giant is not sharply-defined, as depicted in many illustrations. Instead, due to the very low mass density of the envelope, such stars lack a well-defined photosphere. The body of the star gradually transitions into a 'corona' with increasing radii.[45]

At right "is a NASA Hubble Space Telescope image of the cool red giant star Mira A (right), officially called Omicron Ceti in the constellation Cetus, and its nearby hot companion (left) taken on December 11, 1995 in visible light using the European Space Agency's Faint Object Camera (FOC). The stars in this false-color picture are separated by an angular size of only 0.6 arcseconds (equal to 70 times the distance between Earth and the Sun), but clearly resolved by the FOC. Image reconstruction techniques have been used to further enhance the details in the Mira images."[46]

The Hubble Space Telescope (HST) ultraviolet images and later X-ray images by the Chandra space telescope show a spiral of gas rising off Mira in the direction of Mira B. The companion's orbital period around Mira is approximately 400 years.

Mira B, also known as VZ Ceti, is the companion star to the variable star Mira. Its orbit around Mira is poorly known; the most recent estimate listed in the Sixth Orbit Catalog of Visual Binary Stars gives an orbital period of roughly 500 years, with a periastron around the year 2285. Assuming the distance in the Hipparcos catalog and orbit are correct, Mira A and B are separated by an average of 100 AU.

Long-known to be erratically variable itself, its fluctuations seem to be related to its accretion of matter from Mira's stellar wind, which makes it a symbiotic star.[47][48]

The new data suggest that Mira B is a normal main sequence star of spectral type K and roughly 0.7 solar masses, rather than a white dwarf as first envisioned.[49]

Even more recently (2010) analysis of rapid optical brightness variations has indicated that Mira B is in fact a white dwarf.[50]

## Betelgeuse

Betelgeuse is imaged in ultraviolet light by the Hubble Space Telescope and subsequently enhanced by NASA.[51] Credit: NASA and ESA.
This image is from ESO's Very Large Telescope showing not only the stellar disk, but also an extended atmosphere with a previously unknown plume of surrounding gas.[52] Credit: ESO/P. Kervella.

"The yellow/red "image" or "photo" of Betelgeuse usually seen is actually not a picture of the red giant but rather a mathematically generated image based on the photograph. The photograph was actually of much lower resolution: The entire Betelgeuse image fit entirely within a 10x10 pixel area on the Hubble Space Telescopes Faint Object Camera. The actual images were oversampled by a factor of 5 with bicubic spline interpolation, then deconvolved."[51]

The image at the right is "of the supergiant star Betelgeuse obtained with the NACO adaptive optics instrument on ESO’s Very Large Telescope. The use of NACO combined with a so-called “lucky imaging” technique, allows the astronomers to obtain the sharpest ever image of Betelgeuse, even with Earth’s turbulent, image-distorting atmosphere in the way. The resolution is as fine as 37 milliarcseconds, which is roughly the size of a tennis ball on the International Space Station (ISS), as seen from the ground. The image is based on data obtained in the near-infrared, through different filters. The field of view is about half an arcsecond wide, North is up, East is left."[53]

## W Ursae Majoris

The W Ursae Majoris system consists of a pair of stars in a tight, circular orbit with a period of 0.3336 days, or eight hours and 23 seconds.[54] During every orbital cycle, each star eclipses the other, resulting in a decrease in magnitude. The maximum magnitude of the pair is 7.75. During the eclipse of the primary, the net magnitude drops by 0.73, while the eclipse of the secondary causes a magnitude decrease of 0.68.[55] Unlike normal eclipsing binaries, the contact nature makes it impossible to precisely tell when an eclipse of one component by the other starts or ends.

"The two stars in W Ursae Majoris are so close together that their outer envelopes are in direct contact. Hence they have the same stellar classification of F8Vp, which matches the spectrum of a main sequence star that is generating energy through the nuclear fusion of hydrogen. However, the primary component has a larger mass and radius than the secondary, with 1.19 times the Sun's mass and 1.08 times the Sun's radius. The secondary has 0.57 solar masses and 0.78 solar radii.[54][56]

"The orbital period of the system has changed since 1903, which may be the result of mass transfer or the braking effects of magnetic fields. Star spots have been observed on the surface of the stars and strong X-ray emissions have been detected, indicating a high level of magnetic activity that is common to W Uma variables. This magnetic activity may play a role in regulating the timing and magnitude of mass transfer occurs.[57]

## V1010 Ophiuchi

These are light curves for the V1010 Ophiuchi system. Credit: Kam-Ching Leung and Robert E. Wilson.
This diagram shows the contact configuration of V1010 Ophiuchi. Credit: Kam-Ching Leung and Robert E. Wilson.

Def. binaries "in which the stellar components are close enough that proximity effects are important but far enough apart that a large temperature differential may be maintained between the two stars" are called near-contact binaries.[58]

"V1010 Oph ... is one of the brightest and best studied of the near-contact (P=0.66d) binaries."[58] "The period of the binary is known to be decreasing ..., which can be understood in terms of conservative mass transfer (Shaw 1990)."[58] "If this star is truly an evolved system, it may have been in contact previously. ... [I]t is not now in contact"[58].

The temperatures of the two stars have been estimated spectrally as 8200 K and 5671 ± 30 K.[59]

The first image at the right contains two light curves for V1010 Ophiuchi: the top is in yellow at 550.0 nm and the bottom is in blue at 435.0 nm.[59]

The "eclipses are complete and the primary minimum is a transit [...] The system is in contact [shown in the second diagram at the right], with a surface potential near that of the inner contact surface [...] The temperature difference (2529 K) between the primary and secondary is quite large. This suggests that the temperature gradient at the interface must be very steep."[59]

"The appreciable departure between the theoretical light curves and the observations [in the first figure at the right] at the ascending branch of the secondary minimum is due to [a large asymmetry from absorbing gaseous matter]."[59]

"There are two likely ways to form contact systems:

1. through star fission with critical angular momentum, i.e. the angular momentum is just right for the star to divide, but not large enough for it to be detached (zero-age contact);
2. through mass exchange in which one or both components expand to fill the common envelope during the course of stellar evolution."[59]

"V1010 Oph has essentially a ZAMS radius. Thus this system is likely to be essentially a zero-age contact system [formed through star fission]."[59]

## BH Centauri

"The eclipsing binary system BH Cen is a close (contact) binary in the extremely young galactic cluster Córdoba XXVI (NGC 2944)."[60]

In 1928-30, "from ten light minima ... a (half) period P = 0.395790 7 [days is derived]."[61][62] This half period estimate becomes the period P = 0.791 581 4 d,[12] for the observations in 1928-30.

From more recent observations around 1977, P = 0.791 616 d.[16] And, from 1979, P = 0.791 592 10 ± 0.000 14.[60]

## Beta Lyrae

"This video shows the aperture sythesis images of the Beta Lyrae system observed by the CHARA interferometer with the MIRC instrument. The brighter component is the primary star, or the mass donor. The fainter component is the disk surrounding the secondary star, or the mass gainer. The two components are separated by 1 milli-arcsecond. Credit: Ming Zhao, Zhao et al. ApJ 684, L95.

Beta Lyrae is a semidetached binary system made up of a stellar class B7II primary star and a secondary that is probably also a B-type star. The brighter, less massive star (B7II) in the system was once the more massive member of the pair, which caused it to evolve away from the main sequence first and become a giant star. Because the pair are in a close orbit, as this star expanded into a giant it filled its Roche lobe and transferred most of its mass over to its companion. The secondary, now more massive star is surrounded by an accretion disk from this mass transfer, with bipolar, jet-like features projecting perpendicular to the disk.[63] This accretion disk blocks our view of the secondary star, lowering its apparent luminosity and making it difficult for astronomers to pinpoint what its stellar type is. The amount of mass being transferred between the two stars is about 2 × 10–5 solar masses per year, or the equivalent of the Sun's mass every 50,000 years, which results in a increase in orbital period of about 19 seconds each year.[63]

The orbital plane of this system is nearly aligned with the line of sight from the Earth, so the two stars periodically eclipse each other. This causes Beta Lyrae to regularly change its apparent magnitude from +3.4 to +4.6 over an orbital period of 12.9414 days. The two components are so close together that they cannot be resolved with optical telescopes, forming a spectroscopic binary. In 2008, the primary star and the accretion disk of the secondary star were resolved and imaged using the CHARA Array interferometer[64] and the Michigan InfraRed Combiner (MIRC)[65] in the near infrared H band (see video [at the right], allowing the orbital elements to be computed for the first time.[63]

Plaskett's Star (HR 2422) is a spectroscopic binary at a distance of [5,245] light-years (1,608 pc)[66]. It is one of the most massive binary stars known, with components: A = 54 Mʘ[67] and B = 56 Mʘ[67] for a total mass of around [110 Mʘ].[67] The pair have a combined visual magnitude of 6.06[68], and is located in the constellation of Monoceros. The orbital period for the pair is 14.39625 ± 0.00095 days.[67] The secondary is a rapid rotator with a projected rotational velocity of 300 km sec–1,[69] giving it a pronounced equatorial bulge.[67] Plaskett’s star is an example of fission.[30]

## Solar-like binaries

This is a Keck adaptive optics image of TYC 4110-01037-1 in K′. Credit: Keith Matthews at the Keck Observatory.

For a solar-like binary system, the primary has Teff ≲ 6000 K.[70]

"TYC 4410-01037-1 [has] a mass of 1.07 ± 0.08 M and radius of 0.99 ± 0.18 R. ... Teff = 5879 ± 29 K [and] [Fe/H] = -0.01 ± 0.05".[70]

At right is a Keck adaptive optics image of TYC 4110-01037-1 in K′. A faint candidate tertiary companion (indicated by the arrow) with red colors is separated by 986 ± 4 mas from the primary star. If it is physically associated with the primary, it is most likely a dM3-dM4 star. The companion is designated MARVELS-3B.

Its "low-mass stellar companion [has a] small mass ratio [ q ≥ 0.087 ± 0.003] and short orbital period [78.994 ± 0.012 days, which] are atypical amongst solar-like ... binary systems. [The orbit has] an eccentricity of 0.1095 ± 0.0023, and a semi-amplitude of 4199 ± 11 m s-1. ... the minimum companion mass (if sin i = 1) [is] 97.7 ± 5.8 MJup."[70]

"One possible way to create such a system would be if a triple-component stellar multiple broke up into a short period, low q binary during the cluster dispersal phase of its lifetime. A candidate tertiary body has been identified in the system via single-epoch, high contrast imagery. If this object is confirmed to be co-moving, ... it [may] be a dM4 star."[70]

## H I regions

The warm neutral medium (WNM) is 10-20 % of the ISM, ranges in size from 300-400 pc, temperature between 6000 and 10000 K, is composed of neutral atomic hydrogen, has a density of 0.2-0.5 atoms/cm3, and emits the hydrogen 21 cm line.[71]

Also, within the H I regions is the warm ionized medium (WIM), constituting 20-50 % by volume of the ISM, with a size around 1000 pc, a temperature of 8000 K, an atom density of 0.2-0.5 atoms/cm3, of ionized hydrogen, emitting the hydrogen alpha line and exhibiting pulsar dispersion.[71]

These regions are non-luminous, save for emission of the 21-cm (1,420 MHz) region spectral line. Mapping H I emissions with a radio telescope is a technique used for determining the structure of spiral galaxies.

## Molecular clouds

A molecular cloud, sometimes called a stellar nursery if star formation is occurring within, is a type of interstellar cloud whose density and size permits the formation of molecules, most commonly molecular hydrogen (H2).

Molecular hydrogen is difficult to detect by infrared and radio observations, so the molecule most often used to determine the presence of H2 is CO (carbon monoxide). The ratio between CO luminosity and H2 mass is thought to be constant, although there are reasons to doubt this assumption in observations of some other galaxies.[72]

Such clouds make up < 1% of the ISM, have temperatures of 10-20 K and high densities of 102 - 106 atoms/cm3. These clouds are astronomical radio and infrared sources with radio and infrared molecular emission and absorption lines.

## Giant molecular clouds

A vast assemblage of molecular gas with a mass of approximately 103–107 times the mass of the Sun [See, e.g., Table 1 and the Appendix][73] is called a giant molecular cloud (GMC). GMCs are ≈15–600 light-years in diameter (5–200 parsecs).[73] Whereas the average density in the solar vicinity is one particle per cubic centimetre, the average density of a GMC is 102–103 particles per cubic centimetre. Although the Sun is much denser than a GMC, the volume of a GMC is so great that it contains much more mass than the Sun. The substructure of a GMC is a complex pattern of filaments, sheets, bubbles, and irregular clumps.[74]

The densest parts of the filaments and clumps are called "molecular cores", whilst the densest molecular cores are, unsurprisingly, called "dense molecular cores" and have densities in excess of 104–106 particles per cubic centimeter. Observationally molecular cores are traced with carbon monoxide and dense cores are traced with ammonia. The concentration of dust within molecular cores is normally sufficient to block light from background stars so that they appear in silhouette as dark nebulae.[75]

GMCs are so large that "local" ones can cover a significant fraction of a constellation; thus they are often referred to by the name of that constellation, e.g. the Orion Molecular Cloud (OMC) or the Taurus Molecular Cloud (TMC). These local GMCs are arrayed in a ring in the neighborhood of the Sun coinciding with the Gould Belt.[76] The most massive collection of molecular clouds in the galaxy forms an asymmetrical ring around the galactic center at a radius of 120 parsecs; the largest component of this ring is the Sagittarius B2 complex. The Sagittarius region is chemically rich and is often used as an exemplar by astronomers searching for new molecules in interstellar space.[77]

## H II regions

The image is a three-color composite of the sky region of Messier 17. Credit: ESO.
This image is a near-infrared, colour-coded composite image of a sky field in the south-western part of the galactic star-forming region Messier 17. Credit: European Southern Observatory.

An H II region is a large, low-density cloud of partially ionized gas in which star formation has recently taken place.

At right is an image in three-color infrared of an H II region excited by a cluster of young, hot stars. The region is in Messier 17 (M 17). A large silhouette disc occurs to the southwest of the cluster center. This image is obtained with the ISAAC near-infrared instrument at the 8.2-m VLT ANTU telescope at Paranal.

At second right "is a near-infrared, colour-coded composite image of a sky field in the south-western part of the galactic star-forming region Messier 17. In this image, young and heavily obscured stars are recognized by their red colour. Bluer objects are either foreground stars or well-developed massive stars whose intense light ionizes the hydrogen in this region. The diffuse light that is visible nearly everywhere in the photo is due to emission from hydrogen atoms that have (re-)combined from protons and electrons. The dark areas are due to obscuration of the light from background objects by large amounts of dust — this effect also causes many of those stars to appear quite red. A cluster of young stars in the upper-left part of the photo, so deeply embedded in the nebula that it is invisible in optical light, is well visible in this infrared image. Technical information : The exposures were made through three filtres, J (at wavelength 1.25 µm; exposure time 5 min; here rendered as blue), H (1.65 µm; 5 min; green) and Ks (2.2 µm; 5 min; red); an additional 15 min was spent on separate sky frames. The seeing was 0.5 - 0.6 arcsec. The objects in the uppermost left corner area appear somewhat elongated because of a colour-dependent aberration introduced at the edge by the large-field optics. The sky field shown measures approx. 5 x 5 arcmin 2 (corresponding to about 3% of the full moon). North is up and East is left."[78]

## Hypotheses

1. A star or protostar can fission into two or more parts subject to the separability of its interior.

## References

1. Anthony Whitworth, Dimitri Stamatellos, Steffi Walch, Murat Kaplan, Simon Goodwin, David Hubber and Richard Parker (2009). R. de Grijs & J. R. D. Lépine. ed. The formation of brown dwarfs, In: Star clusters: basic galactic building blocks, Proceedings IAU Symposium No. 266. International Astronomical Union. pp. 264-71. doi:10.1017/S174392130999113X. Retrieved 2011-10-30.
2. M. A. Dopita, L. J. Kewley, C. A. Heisler, and R. S. Sutherland (October 2000). "A Theoretical Recalibration of the Extragalactic H II Region Sequence". The Astrophysical Journal 542 (1): 224-34. doi:10.1086/309538.
3. Biermann, P. L.; Langer, N.; Seo, Eun-Suk; Stanev, T. (April 2001). "Cosmic rays IX. Interactions and transport of cosmic rays in the Galaxy". Astronomy and Astrophysics 369 (4): 269-77. doi:10.1051/0004-6361:20010083.
4. Zero Age Main Sequence, In: The SAO Encyclopedia of Astronomy. Swinburne University. Retrieved 2012-03-24.
5. J. A. O'Keefe (1975). "Secularly Unstable Maclaurin Ellipsoids and the Pre-Fission State of the Earth". Bulletin of the American Astronomical Society 7: 384-5.
6. L. A. Molnar (2011). Size and Age Dependence of Koronis Family Colors (PDF). 6. EPSC Abstracts. p. 2. Retrieved 2014-04-13.
7. A. Carpinteri and A. Manuello (2011). "Geomechanical and Geochemical Evidence of Piezonuclear Fission Reactions in the Earth's Crust". Strain 47 (Supplement 2): 267-81. doi:10.1111/j.1475-1305.2010.00766.x/full. Retrieved 2014-04-13.
8. Joel E. Tohline (September 2002). "The Origin of Binary Stars". Annual Review of Astronomy and Astrophysics 40 (1): 349-85. doi:10.1146/annurev.astro.40.060401.093810. Retrieved 2013-10-23.
9. Keke Zhang, Xinhao Liao, and Gerald Schubert (March 10, 2003). "Nonaxisymmetric Instabilities of a Toroidal Magnetic Field in a Rotating Sphere". The Astrophysical Journal 585 (2): 1124-37. Retrieved 2014-04-12.
10. p. 231, Stellar Rotation, Jean Louis Tassoul, Andrew King, Douglas Lin, Stephen P. Maran, Jim Pringle, and Martin Ward, Cambridge, UK, New York: Cambridge University Press, 2000. ISBN 0-521-77218-4.
11. p. 19, Double and Multiple Stars and how to Observe Them, James Mullaney, New York, London: Springer, 2005. ISBN 1-85233-751-6.
12. Kam-Ching Leung and Donald P. Schneider (February 1977). "Eclipsing systems in star clusters. III. Early-type contact system BH Centauri". The Astrophysical Journal 211 (2): 844-52. doi:10.1086/154993.
13. contact binary, David Darling, The Internet Encyclopedia of Science. Accessed on line November 4, 2007.
14. overcontact binary, David Darling, The Internet Encyclopedia of Science. Accessed on line November 4, 2007.
15. pp. 51–53, An Introduction to Astrophysical Fluid Dynamics, Michael J. Thompson, London: Imperial College Press, 2006. ISBN 1-86094-615-1.
16. Kam-Ching Leung, R. F. Sistero, Di-Sheng Zhai, A. Grieco, B. Candellero (June 1984). "Revised UBV photometric solution of the early-type contact system BH Centauri". The Astronomical Journal 89 (6): 872-5. doi:10.1086/113582.
17. K.-C. Leung and R. E. Wilson (1976). P. Eggleton. ed. An Aspect of Star Fission, In: Structure and Evolution of Close Binary Systems; Proceedings of the Symposium, Cambridge, England, July 28-August 1, 1975. Dordrecht: D. Reidel Publishing Co.. pp. 365-6.
18. Axel Brandenburg, Åke Nordlund, Robert F. Stein, and Ulf Torkelsson (June 1995). "Dynamo-generated Turbulence and Large-Scale Magnetic Fields in a Keplerian Shear Flow". The Astrophysical Journal 446 (6): 741-54. doi:10.1086/175831.
19. P. Petit, F. Lignières, G.A. Wade, M. Aurière, T. Böhm, S. Bagnulo, B. Dintrans, A. Fumel, J. Grunhut, J. Lanoux, A. Morgenthaler, and V. Van Grootel (November-December 2010). "The rapid rotation and complex magnetic field geometry of Vega". Astronomy and Astrophysics 523 (11): A41-9. doi:10.1051/0004-6361/201015307. Retrieved 2011-12-19.
20. Iben, Icko, Jr. (1991). "Single and binary star evolution". Astrophysical Journal Supplement Series 76: 55–114. doi:10.1086/191565.
21. Szebehely, Victor G.; Curran, Richard B. (1985). Stability of the Solar System and Its Minor Natural and Artificial Bodies. Springer. ISBN 90-277-2046-0.
22. Cathie Clarke (January 1995). "Theories for Binary Star Formation". Astrophysics and Space Science 223 (1-2): 73-86. doi:10.1007/BF00989156.
23. A. Maeder (May 1987). "Evidences for a bifurcation in massive star evolution. The ON-blue stragglers". Astronomy and Astrophysics 178 (1-2): 159-69.
24. James Hopwood Jeans (1929). Astronomy and Cosmogeny. Cambridge: Cambridge University Press. p. 400. Retrieved 2012-03-24.
25. Myron A. Smith, Jacques M. Beckers, and Samuel C. Barden (August 1983). "Rotation among Orion IC G stars-Angular momentum loss considerations in pre-main-sequence stars". The Astrophysical Journal 271 (8): 237-54. doi:10.1086/161190.
26. Helmut A. Abt (1981). T. Gehrels. ed. [adsabs.harvard.edu/abs/1978prpl.conf..323A The binary frequency along the main sequence, In: Protostars and Planets]. Tucson, Arizona: University of Arizona Press. pp. 323. adsabs.harvard.edu/abs/1978prpl.conf..323A. Retrieved 2012-03-24.
27. Helmut A. Abt, Ana E. Gomez, and Saul G. Levy (October 1990). "The frequency and formation mechanism of B2-B5 main-sequence binaries". The Astrophysical Journal Supplement Series 74 (10): 551-73. doi:10.1086/191508.
28. L. B. Lucy (December 1977). "A numerical approach to the testing of the fission hypothesis". Astronomical Journal 82 (12): 1013-24. doi:10.1086/112164.
29. J. H. Jeans (March 1927). "On liquid stars and the liberation of stellar energy". Monthly Notices of the Royal Astronomical Society 87 (3): 400-14.
30. Otto Struve (June 1952). "Notes on stellar spectra, III". Publications of the Astronomical Society of the Pacific 67 (375): 117-21. doi:10.1086/126441.
31. A.P. Boss (1992). J. Sahade; G.E. McCluskey; Yoji Kondo (eds.). Formation of Binary Stars, In: The Realm of Interacting Binary Stars. Dordrecht: Kluwer Academic. p. 355. ISBN 0-7923-1675-4. Retrieved 2012-03-24.
32. J.E. Tohline, J.E. Cazes, H.S. Cohl. The Formation of Common-Envelope, Pre-Main-Sequence Binary Stars. Louisiana State University. Retrieved 2012-03-24.CS1 maint: multiple names: authors list (link)
33. J. E. Pringle (July 1989). "On the formation of binary stars". Royal Astronomical Society, Monthly Notices 239 (7): 361-70.
34. Melissa L. Enoch, Neal J. Evans II, Anneila I. Sargent, and Jason Glenn (February 20, 2009). "Properties of the youngest protostars in Perseus, Serpens, and Ophiuchus". The Astrophysical Journal 692 (2): 973-97. doi:10.1088/0004-637X/692/2/973. Retrieved 2013-12-20.
35. Cataclysmic Variables. NASA Goddard Space Flight Center. 2004-11-01. Retrieved 2006-06-08.
36. Daniel Clery (6 January 2017). Colliding stars will light up the night sky in 2022. Science Magazine. Retrieved 2017-01-14.
37. Phil Plait (June 29, 2012). Cannonball star blasts away from the scene of the crime. Discover, The Magazine of Science, Technology, and the Future. Retrieved 2013-03-10.
38. J. Tomsick; et al. (June 28, 2012). IGR J11014-6103: Has the Speediest Pulsar Been Found?. 60 Garden Street, Cambridge, MA 02138 USA: Harvard-Smithsonian Center for Astrophysics. Retrieved 2013-03-10.CS1 maint: location (link)
39. Simon Albrecht, J.N. Winn, D. C. Fabrycky, G. Torres, and J. Setiawan (2011). Mercedes T. Richards & Ivan Hubeny. ed. The BANANA Survey: Spin-Orbit Alignment in Binary Stars, In: Interacting Binaries to Exoplanets: Essential Modeling Tools. 282. Cambridge University Press. pp. 397-8. Retrieved 2014-04-13.
40. O. Manuel, C. Bolon, A. Katragada, and M. Insall (2001). "Attraction and Repulsion of Nucleons: Sources of Stellar Energy". Journal of Fusion Energy 19 (1): 93-8. doi:10.1023/A:1012290028638. Retrieved 2014-04-13.
41. W. D. Harkins (2001). "Attraction and Repulsion of Nucleons: Sources of Stellar Energy". Journal of Fusion Energy 19 (1): 93-8. doi:10.1023/A:1012290028638. Retrieved 2014-04-13.
42. J. Marvin Herndon (May 9 1994). "Planetary and Protostellar Nuclear Fission: Implications for Planetary Change, Stellar Ignition and Dark Matter". Proceedings of the Royal Society A Mathematical, Physical & Engineering Sciences 445 (1924): 453-61. doi:10.1098/rspa.1994.0071. Retrieved 2014-04-13.
43. Peter Bodenheimer (1995). "Angular Momentum Evolution of Young Stars and Disks". Annual Review of Astronomy and Astrophysics 33: 199-238. doi:10.1146/annurev.aa.33.090195.001215. Retrieved 2014-04-15.
44. The Illustrated Oxford Dictionary, Oxford University Press, 1998
45. orange sphere of the sun
46. Margarita Karovska (August 6, 1997). Hubble Separates Stars in the Mira Binary System. Harvard-Smithsonian Center for Astrophysics, Boston, Massachusetts: STSci and NASA. Retrieved 2012-08-06.
47. Robert Burnham, Jr., Burnham's Celestial Handbook, Vol. 1, (New York: Dover Publications, Inc., 1978), 637-8.
48. James Kaler, The Hundred Greatest Stars, (New York: Copernicus Books, 2002), 121.
49. First Planet-Forming Disk Found in the Environment of a Dying Star. Retrieved 10 January 2007.
50. Sokoloski and Lars Bildsten (2010). Evidence for the White Dwarf Nature of Mira B.
51. Ronald L. Gilliland, Andrea K. Dupree (May 1996). "First Image of the Surface of a Star with the Hubble Space Telescope" (PDF). Astrophysical Journal Letters 463 (1): L29-32. doi:10.1086/310043. Retrieved 1 August 2010.
52. Robert Nemiroff (MTU) & Jerry Bonnell (USRA) (5 August 2009). "Betelgeuse Resolved". Today's Astronomy Picture of the Day. Retrieved 17 November 2010.
53. P. Kervella (July 29, 2009). A close look at Betelgeuse. Santiago, Chile: European Southern Observatory. Retrieved 2012-07-11.
54. S. Bilir, Y. Karataş, O. Demircan, Z. Eker (February 2005). "Kinematics of W Ursae Majoris type binaries and evidence of the two types of formation". Monthly Notices of the Royal Astronomical Society 357 (2): 497–517. doi:10.1111/j.1365-2966.2005.08609.x.
55. O. Yu. Malkov, E. Oblak, E. A. Snegireva, J. Torra (February 2006). "A catalogue of eclipsing variables". Astronomy and Astrophysics 446 (2): 785–789. doi:10.1051/0004-6361:20053137.
56. Gazeas, K.; Stȩpień, K. (November 2008). "Angular momentum and mass evolution of contact binaries". Monthly Notices of the Royal Astronomical Society 390 (4): 1577–1586. doi:10.1111/j.1365-2966.2008.13844.x.
57. Morgan, N.; Sauer, M.; Guinan, E. (1997). "New Light Curves and Period Study of the Contact Binary W Ursae Majoris". Information Bulletin on Variable Stars 4517: 1.
58. M. F. Corcoran, M. J. Siah, E. F. Guinan (May 1991). "Hβ Photometry of V1010 Ophiuchi". The Astrophysical Journal 101 (5): 1828-34. doi:10.1086/115810. Retrieved 2012-08-06.
59. Kam-Ching Leung and Robert E. Wilson (February 1, 1977). "The Early-Type Contact System V1010 Ophiuchi". The Astrophysical Journal 211 (02): 853-8. doi:10.1086/154994. Retrieved 2014-04-11.
60. R. F. Sistero, A. Grieco, and B. Candellero (April 1983). "The early-contact system BH Centauri - UBV photometry". Astrophysics and Space Science 91 (2): 427-33. Retrieved 2012-08-06.
61. P. Th. Oosterhoff (June 27, 1928). "First ephemerides of 25 variable stars". Bulletin of the Astronomical Institutes of the Netherlands 4 (148): 183-94.
62. P. Th. Oosterhoff (April 1930). "Improved elements of 7 variable stars". Bulletin of the Astronomical Institutes of the Netherlands 5 (184): 156.
63. M. Zhao, D. Gies, J. D. Monnier, N. Thureau, E. Pedretti, F. Baron, A. Merand, T. ten Brummelaar, H. McAlister (September 2008). "First Resolved Images of the Eclipsing and Interacting Binary β Lyrae". The Astrophysical Journal 684 (2): L95–8. doi:10.1086/592146.
64. ten Brummelaar, Theo; et al. (2005), "First Results from the CHARA Array. II. A Description of the Instrument", The Astrophysical Journal, 628 (453), arXiv:astro-ph/0504082, Bibcode:2005ApJ...628..453T, doi:10.1086/430729 Unknown parameter |month= ignored (help)
65. Monnier, John D.; et al. (2006), "Michigan Infrared Combiner (MIRC): commissioning results at the CHARA Array", Proceedings of the SPIE, 6268 (62681P), Bibcode:2006SPIE.6268E..55M, doi:10.1117/12.671982
66. A. Megier, A. Strobel, G. A. Galazutdinov, J. Krełowski (November 2009). "The interstellar Ca II distance scale". Astronomy and Astrophysics 507 (2): 833–840. doi:10.1051/0004-6361/20079144.
67. N. Linder, G. Rauw, F. Martins, H. Sana , M. De Becker, E. Gosset (October 2008). "High-resolution optical spectroscopy of Plaskett's star". Astronomy and Astrophysics 489 (2): 713–723. doi:10.1051/0004-6361:200810003.
68. H. L. Johnson, B. Iriarte, R. I. Mitchell, W. Z. Wisniewskj (1966). "UBVRIJKL photometry of the bright stars". Communications of the Lunar and Planetary Laboratory 4 (99).
69. L. Mahy, E. Gosset, F. Baudin, G. Rauw, M. Godart, T. Morel, P. Degroote, C. Aerts, R. Blomme (January 2011). "Plaskett's star: analysis of the CoRoT photometric data". Astronomy and Astrophysics 525: A101. doi:10.1051/0004-6361/201014777.
70. John P. Wisniewski, Jian Ge, Justin R. Crepp, Nathan De Lee, Jason Eastman, Massimiliano Esposito, Scott W. Fleming, B. Scott Gaudi, Luan Ghezzi, Jonay I. Gonzalez Hernandez, Brian L. Lee, Keivan G. Stassun, Eric Agol, Carlos Allende Prieto, Rory Barnes, Dmitry Bizyaev, Phillip Cargile, Liang Chang, Luiz N. DaCosta, G.F. Porto De Mello, Bruno Femenía, Leticia D. Ferreira, Bruce Gary, Leslie Hebb, Jon Holtzman, Jian Liu, Bo Ma, Claude E. Mack III, Suvrath Mahadevan, Marcio A.G. Maia, Duy Cuong Nguyen, Ricardo L.C. Ogando, Daniel J. Oravetz, Martin Paegert, Kaike Pan, Joshua Pepper, Rafael Rebolo, Basilio Santiago, Donald P. Schneider, Alaina C Shelden, Audrey Simmons, Benjamin M. Tofflemire, Xiaoke Wan, Ji Wang, Bo Zhao (May 2012). "Very Low-Mass Stellar and Substellar Companions to Solar-like Stars from MARVELS I: a Low Ratio Stellar Companion to TYC 4110-01037-1 in a 79-day Orbit". Astronomical Journal 143 (5): 107-18. doi:10.1088/0004-6256/143/5/107. Retrieved 2013-08-05.
71. K. Ferriere (2001). "The Interstellar Environment of our Galaxy". Reviews of Modern Physics 73 (4): 1031–66. doi:10.1103/RevModPhys.73.1031.
72. Craig Kulesa. Overview: Molecular Astrophysics and Star Formation. Research Projects. Retrieved September 7, 2005.
73. Norman Murray (March 2011). "Star Formation Efficiencies and Lifetimes of Giant Molecular Clouds in the Milky Way". The Astrophysical Journal 729 (2): 14. doi:10.1088/0004-637X/729/2/133. Retrieved 2016-10-07.
74. J. P. Williams, L. Blitz, C. F. McKee (2000). The Structure and Evolution of Molecular Clouds: from Clumps to Cores to the IMF, In: Protostars and Planets IV. Tucson: University of Arizona Press. p. 97.CS1 maint: multiple names: authors list (link)
75. Di Francesco, J.; et al. (2006). An Observational Perspective of Low-Mass Dense Cores I: Internal Physical and Chemical Properties, In: Protostars and Planets V.
76. Sagittarius B2 and its Line of Sight
77. ESO00 (September 14, 2000). Peering into a Star Factory. Paranal: European Southern Observatory. Retrieved 2013-03-14.