Wikipedia

IK Pegasi

IK Pegasi (or HR 8210) is a binary star system in the constellation Pegasus. It is just luminous enough to be seen with the unaided eye, at a distance of about 154 light years from the Solar System.

IK Pegasi

Location of IK Pegasi.
Observation data
Epoch J2000      Equinox J2000
Constellation Pegasus
Right ascension 21h 26m 26.66066s[1]
Declination +19° 22′ 32.3169″[1]
Apparent magnitude (V) 6.08[2]
Characteristics
A
Spectral type A8m:[3] or kA6hA9mF0[4]
U−B color index 0.03[5]
B−V color index 0.235±0.009[2]
Variable type Delta Scuti[3]
B
Spectral type DA[6]
Astrometry
Radial velocity (Rv)−9.7±0.2[2] km/s
Proper motion (μ) RA: +80.964[1] mas/yr
Dec.: +16.205[1] mas/yr
Parallax (π)21.1287 ± 0.1410 mas[1]
Distance154 ± 1 ly
(47.3 ± 0.3 pc)
Absolute magnitude (MV)2.75[2]
Details
A
Mass1.65[7] M☉
Radius1.47+0.07
−0.09[1] R☉
Luminosity6.568±0.051[1] L☉
Surface gravity (log g)4.25[7] cgs
Temperature7,624+237
−181[1] K
Metallicity117[7][8]
Rotational velocity (v sin i)< 32.5[8] km/s
Age50–600[7] Myr
B
Mass1.15[9] M☉
Radius0.006[6] R☉
Luminosity0.12[nb 1] L☉
Surface gravity (log g)8.95[6] cgs
Temperature35,500[9] K
Other designations
AB: IK Peg, BD+18° 4794, HD 204188, HIP 105860, HR 8210, SAO 107138.[5]
B: WD 2124+191, EUVE J2126+193.[10][11]
Database references
SIMBADdata

The primary (IK Pegasi A) is an A-type main-sequence star that displays minor pulsations in luminosity. It is categorized as a Delta Scuti variable star and it has a periodic cycle of luminosity variation that repeats itself about 22.9 times per day.[7] Its companion (IK Pegasi B) is a massive white dwarf—a star that has evolved past the main sequence and is no longer generating energy through nuclear fusion. They orbit each other every 21.7 days with an average separation of about 31 million kilometres, or 19 million miles, or 0.21 astronomical units (AU). This is smaller than the orbit of Mercury around the Sun.

IK Pegasi B is the nearest known supernova progenitor candidate. When the primary begins to evolve into a red giant, it is expected to grow to a radius where the white dwarf can accrete matter from the expanded gaseous envelope. When the white dwarf approaches the Chandrasekhar limit of 1.4 solar masses (M☉),[12] it may explode as a Type Ia supernova.[13]

Observation

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This star system was catalogued in the 1862 Bonner Durchmusterung ("Bonn astrometric Survey") as BD +18°4794B. It later appeared in Pickering's 1908 Harvard Revised Photometry Catalogue as HR 8210.[14] The designation "IK Pegasi" follows the expanded form of the variable star nomenclature introduced by Friedrich W. Argelander.[15]

Examination of the spectrographic features of this star showed the characteristic absorption line shift of a binary star system. This shift is created when their orbit carries the member stars toward and then away from the observer, producing a doppler shift in the wavelength of the line features. The measurement of this shift allows astronomers to determine the relative orbital velocity of at least one of the stars even though they are unable to resolve the individual components.[16]

In 1927, the Canadian astronomer William E. Harper used this technique to measure the period of this single-line spectroscopic binary and determined it to be 21.724 days. He also initially estimated the orbital eccentricity as 0.027. (Later estimates gave an eccentricity of essentially zero, which is the value for a circular orbit.)[13] The velocity amplitude was measured as 41.5 km/s, which is the maximum velocity of the primary component along the line of sight to the Solar System.[17]

The distance to the IK Pegasi system can be measured directly by observing the tiny parallax shifts of this system (against the more distant stellar background) as the Earth orbits around the Sun. This shift was measured to high precision by the Hipparcos spacecraft, yielding a distance estimate of 150 light years (with an accuracy of ±5 light years).[18] The same spacecraft also measured the proper motion of this system. This is the small angular motion of IK Pegasi across the sky because of its motion through space.

The combination of the distance and proper motion of this system can be used to compute the transverse velocity of IK Pegasi as 16.9 km/s.[nb 2] The third component, the heliocentric radial velocity, can be measured by the average red-shift (or blue-shift) of the stellar spectrum. The General Catalogue of Stellar Radial Velocities lists a radial velocity of −11.4 km/s for this system.[19] The combination of these two motions gives a space velocity of 20.4 km/s relative to the Sun.[2]

An attempt was made to photograph the individual components of this binary using the Hubble Space Telescope, but the stars proved too close to resolve.[20] Recent measurements with the Extreme Ultraviolet Explorer space telescope gave a more accurate orbital period of 21.72168 ± 0.00009 days.[10] The inclination of this system's orbital plane is believed to be nearly edge-on (90°) as seen from the Earth. If so it may be possible to observe an eclipse.[9]

IK Pegasi A

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A light curve for IK Pegasi, plotted from TESS data[21]

The Hertzsprung–Russell diagram (HR diagram) is a plot of luminosity versus a color index for a set of stars. IK Pegasi A is currently a main sequence star—a term that is used to describe a nearly linear grouping of core hydrogen-fusing stars based on their position on the HR diagram. However, IK Pegasi A lies in a narrow, nearly vertical band of the HR diagram that is known as the instability strip. Stars in this band oscillate in a coherent manner, resulting in periodic pulsations in the star's luminosity.[22]

The pulsations result from a process called the κ-mechanism. A part of the star's outer atmosphere becomes optically thick due to partial ionization of certain elements. When these atoms lose an electron, the likelihood that they will absorb energy increases. This results in an increase in temperature that causes the atmosphere to expand. The inflated atmosphere becomes less ionized and loses energy, causing it to cool and shrink back down again. The result of this cycle is a periodic pulsation of the atmosphere and a matching variation of the luminosity.[22]

 
The relative dimensions of IK Pegasi A (left), B (lower center) and the Sun (right).[23]

Stars within the portion of the instability strip that crosses the main sequence are called Delta Scuti variables. These are named after the prototypical star for such variables: Delta Scuti. Delta Scuti variables typically range from spectral class A2 to F8, and a stellar luminosity class of III (giants) to V (main sequence stars). They are short-period variables that have a regular pulsation rate between 0.025 and 0.25 days. Delta Scuti stars have an abundance of elements similar to the Sun's (see Population I stars) and between 1.5 and 2.5 M☉.[24] The pulsation rate of IK Pegasi A has been measured at 22.9 cycles per day, or once every 0.044 days.[7]

Astronomers define the metallicity of a star as the abundance of chemical elements that have a higher atomic number than helium. This is measured by a spectroscopic analysis of the atmosphere, followed by a comparison with the results expected from computed stellar models. In the case of IK Pegasus A, the estimated metal abundance is [M/H] = +0.07 ± 0.20. This notation gives the logarithm of the ratio of metal elements (M) to hydrogen (H), minus the logarithm of the Sun's metal ratio. (Thus if the star matches the metal abundance of the Sun, this value will be zero.) A logarithmic value of 0.07 is equivalent to an actual metallicity ratio of 1.17, so the star is about 17% richer in metallic elements than the Sun.[7] However the margin of error for this result is relatively large.

The spectrum of A-class stars such as IK Pegasi A show strong Balmer lines of hydrogen along with absorption lines of ionized metals, including the K line of ionized calcium (Ca II) at a wavelength of 393.3 nm.[25] The spectrum of IK Pegasi A is classified as marginal Am (or "Am:"), which means it displays the characteristics of a spectral class A but is marginally metallic-lined. That is, this star's atmosphere displays slightly (but anomalously) higher than normal absorption line strengths for metallic isotopes.[3] Stars of spectral type Am are often members of close binaries with a companion of about the same mass, as is the case for IK Pegasi.[26]

Spectral class-A stars are hotter and more massive than the Sun. But, in consequence, their life span on the main sequence is correspondingly shorter. For a star with a mass similar to IK Pegasi A (1.65 M☉), the expected lifetime on the main sequence is 2–3 × 109 years, which is about half the current age of the Sun.[27]

In terms of mass, the relatively young Altair is the nearest star to the Sun that is a stellar analogue of component A—it has an estimated 1.7 M☉. The binary system as a whole has some similarities to the nearby system of Sirius, which has a class-A primary and a white dwarf companion. However, Sirius A is more massive than IK Pegasi A and the orbit of its companion is much larger, with a semimajor axis of 20 AU.

IK Pegasi B

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The companion star is a dense white dwarf star. This category of stellar object has reached the end of its evolutionary life span and is no longer generating energy through nuclear fusion. Instead, under normal circumstances, a white dwarf will steadily radiate away its excess energy, mainly stored heat, growing cooler and dimmer over the course of many billions of years.[28]

Evolution

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Nearly all small and intermediate-mass stars (below about 8~9 M☉) will end up as white dwarfs once they have exhausted their supply of thermonuclear fuel.[29] Such stars spend most of their energy-producing life span as a main-sequence star. The time that a star spends on the main sequence depends primarily on its mass, with the lifespan decreasing with increasing mass.[30] Thus, for IK Pegasi B to have become a white dwarf before component A, it must once have been more massive than component A. In fact, the progenitor of IK Pegasi B is thought to have had a mass between 5 and 8 M☉.[13]

As the hydrogen fuel at the core of the progenitor of IK Pegasi B was consumed, it evolved into a red giant. The inner core contracted until hydrogen burning commenced in a shell surrounding the helium core. To compensate for the temperature increase, the outer envelope expanded to many times the radius it possessed as a main sequence star. When the core reached a temperature and density where helium could start to undergo fusion this star contracted and became what is termed a horizontal branch star. That is, it belonged to a group of stars that fall upon a roughly horizontal line on the H-R diagram. The fusion of helium formed an inert core of carbon and oxygen. When helium was exhausted in the core a helium-burning shell formed in addition to the hydrogen-burning one and the star moved to what astronomers term the asymptotic giant branch, or AGB. (This is a track leading to the upper-right corner of the H-R diagram.) If the star had sufficient mass, in time carbon fusion could begin in the core, producing oxygen, neon and magnesium.[31][32][33]

The outer envelope of a red giant or AGB star can expand to several hundred times the radius of the Sun, occupying a radius of about 5 × 108 km (3 AU) in the case of the pulsating AGB star Mira.[34] This is well beyond the current average separation between the two stars in IK Pegasi, so during this time period the two stars shared a common envelope. As a result, the outer atmosphere of IK Pegasi A may have received an isotope enhancement.[9]

 
The Helix Nebula is being created by a star evolving into a white dwarf. NASA & ESA image.

Some time after an inert oxygen-carbon (or oxygen-magnesium-neon) core formed, thermonuclear fusion began to occur along two shells concentric with the core region; hydrogen was burned along the outermost shell, while helium fusion took place around the inert core. However, this double-shell phase is unstable, so it produced thermal pulses that caused large-scale mass ejections from the star's outer envelope.[35] This ejected material formed an immense cloud of material called a planetary nebula. All but a small fraction of the hydrogen envelope was driven away from the star, leaving behind a white dwarf remnant composed primarily of the inert core.[36]

Composition and structure

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The interior of IK Pegasi B may be composed wholly of carbon and oxygen; alternatively, if its progenitor underwent carbon burning, it may have a core of oxygen and neon, surrounded by a mantle enriched with carbon and oxygen.[37][38] In either case, the exterior of IK Pegasi B is covered by an atmosphere of almost pure hydrogen, which gives this star its stellar classification of DA. Due to higher atomic mass, any helium in the envelope will have sunk beneath the hydrogen layer.[6] The entire mass of the star is supported by electron degeneracy pressure—a quantum mechanical effect that limits the amount of matter that can be squeezed into a given volume.

 
This graph shows the theoretical radius of a white dwarf, given its mass. The green curve is for a relativistic electron gas model.

At an estimated 1.15 M☉, IK Pegasi B is considered to be a high-mass white dwarf.[nb 3] Although its radius has not been observed directly, it can be estimated from known theoretical relationships between the mass and radius of white dwarfs,[39] giving a value of about 0.60% of the Sun's radius.[6] (A different source gives a value of 0.72%, so there remains some uncertainty in this result.)[7] Thus this star packs a mass greater than the Sun into a volume roughly the size of the Earth, giving an indication of this object's extreme density.[nb 4]

The massive, compact nature of a white dwarf produces a strong surface gravity. Astronomers denote this value by the decimal logarithm of the gravitational force in cgs units, or log g. For IK Pegasi B, log g is 8.95.[6] By comparison, log g for the Earth is 2.99. Thus the surface gravity on IK Pegasi is over 900,000 times the gravitational force on the Earth.[nb 5]

The effective surface temperature of IK Pegasi B is estimated to be about 35,500 ± 1,500 K,[9] making it a strong source of ultraviolet radiation.[6][nb 6] Under normal conditions this white dwarf would continue to cool for more than a billion years, while its radius would remain essentially unchanged.[40]

Future evolution

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In a 1993 paper, David Wonnacott, Barry J. Kellett and David J. Stickland identified this system as a candidate to evolve into a Type Ia supernova or a cataclysmic variable.[13] At a distance of 150 light years, this makes it the nearest known candidate supernova progenitor to the Earth. However, in the time it will take for the system to evolve to a state where a supernova could occur, it will have moved a considerable distance from Earth but may still pose a threat.

At some point in the future, IK Pegasi A will consume the hydrogen fuel at its core and start to evolve away from the main sequence to form a red giant. The envelope of a red giant can grow to significant dimensions, extending up to a hundred times its previous radius (or larger). Once IK Pegasi A expands to the point where its outer envelope overflows the Roche lobe of its companion, a gaseous accretion disk will form around the white dwarf. This gas, composed primarily of hydrogen and helium, will then accrete onto the surface of the companion. This mass transfer between the stars will also cause their mutual orbit to shrink.[41]

On the surface of the white dwarf, the accreted gas will become compressed and heated. At some point the accumulated gas can reach the conditions necessary for hydrogen fusion to occur, producing a runaway reaction that will drive a portion of the gas from the surface. This would result in a (recurrent) nova explosion—a cataclysmic variable star—and the luminosity of the white dwarf would rapidly increase by several magnitudes for a period of several days or months.[42] An example of such a star system is RS Ophiuchi, a binary system consisting of a red giant and a white dwarf companion. RS Ophiuchi has flared into a (recurrent) nova on at least six occasions, each time accreting the critical mass of hydrogen needed to produce a runaway explosion.[43][44]

It is possible that IK Pegasi B will follow a similar pattern.[43] In order to accumulate mass, however, only a portion of the accreted gas can be ejected, so that with each cycle the white dwarf would steadily increase in mass. Thus, even should it behave as a recurring nova, IK Pegasus B could continue to accumulate a growing envelope.[45]

An alternate model that allows the white dwarf to steadily accumulate mass without erupting as a nova is called the close-binary supersoft x-ray source (CBSS). In this scenario, the mass transfer rate to the close white dwarf binary is such that a steady fusion burn can be maintained on the surface as the arriving hydrogen is consumed in thermonuclear fusion to produce helium. This category of super-soft sources consist of high-mass white dwarfs with very high surface temperatures (0.5 × 106 to 1 × 106 K[46]).[47]

Should the white dwarf's mass approach the Chandrasekhar limit of 1.4 M☉ it will no longer be supported by electron degeneracy pressure and it will undergo a collapse. For a core primarily composed of oxygen, neon and magnesium, the collapsing white dwarf is likely to form a neutron star. In this case, only a fraction of star's mass will be ejected as a result.[48] If the core is instead made of carbon-oxygen, however, increasing pressure and temperature will initiate carbon fusion in the center prior to attainment of the Chandrasekhar limit. The dramatic result is a runaway nuclear fusion reaction that consumes a substantial fraction of the star within a short time. This will be sufficient to unbind the star in a cataclysmic, Type Ia supernova explosion.[49]

Such a supernova event may pose some threat to life on the Earth. It is thought that the white dwarf, IK Pegasi B, is unlikely to detonate as a supernova for 1.9 billion years.[50] As shown previously, the space velocity of this star relative to the Sun is 20.4 km/s (12.7 mi/s). This is equivalent to moving a distance of one light year every 14,700 years. After 5 million years, for example, this star will be separated from the Sun by more than 500 light years. A Type Ia supernova within a thousand parsecs (3,300 light-years) is thought to be able to affect the Earth,[51] but it must be closer than about 10 parsecs (around thirty light-years) to cause a major harm to the terrestrial biosphere.[50]

Following a supernova explosion, the remnant of the donor star (IK Pegasus A) would continue with the final velocity it possessed when it was a member of a close orbiting binary system. The resulting relative velocity could be as high as 100–200 km/s (62–124 mi/s), which would place it among the high-velocity members of the galaxy. The companion will also have lost some mass during the explosion, and its presence may create a gap in the expanding debris. From that point forward it will evolve into a single white dwarf star.[52][53] The supernova explosion will create a remnant of expanding material that will eventually merge with the surrounding interstellar medium.[54]

See also

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Notes

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  1. ^ Based upon:
     
    where L is luminosity, R is radius and Teff is the effective temperature. See:
    Krimm, Hans (August 19, 1997). "Luminosity, Radius and Temperature". Hampden-Sydney College. Archived from the original on May 8, 2003. Retrieved 2007-05-16.
  2. ^ The net proper motion is given by:
      mas/y.
    where   and   are the components of proper motion in the RA and Dec., respectively. The resulting transverse velocity is:
    Vt = μ • 4.74 d (pc) = 16.9 km.
    where d(pc) is the distance in parsecs. See:
    Majewski, Steven R. (2006). "Stellar Motions". University of Virginia. Archived from the original on 2012-01-25. Retrieved 2007-05-14.
  3. ^ The white-dwarf population is narrowly distributed around the mean mass of 0.58 M☉, and only 2%. See:
    Holberg, J. B.; Barstow, M. A.; Bruhweiler, F. C.; Cruise, A. M.; et al. (1998). "Sirius B: A New, More Accurate View". The Astrophysical Journal. 497 (2): 935–942. Bibcode:1998ApJ...497..935H. doi:10.1086/305489. of all white dwarfs have at least one solar mass.
  4. ^ R* = 0.006 • (6.96 × 108) ≈ 4,200 km.
  5. ^ The surface gravity of the Earth is 9.780 m/s2, or 978.0 cm/s2 in cgs units. Thus:
     
    The log of the gravitational force ratios is 8.95 - 2.99 = 5.96. So:
     
  6. ^ From Wien's displacement law, the peak emission of a black body at this temperature would be at a wavelength of:
      nm
    which lies in the far ultraviolet part of the electromagnetic spectrum.

References

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  1. ^ a b c d e f g h Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. ^ a b c d e Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID 119257644.
  3. ^ a b c Kurtz, D. W. (1978), "Metallicism and pulsation - The marginal metallic line stars", Astrophysical Journal, 221: 869–880, Bibcode:1978ApJ...221..869K, doi:10.1086/156090, hdl:2152/34842
  4. ^ Skiff, B. A. (October 2014), "Catalogue of Stellar Spectral Classifications", Lowell Observatory, VizieR On-line Data Catalog: B/mk, Bibcode:2014yCat....1.2023S.
  5. ^ a b "HD 12139". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-11-13. — Note: some results were queried via the "Display all measurements" function on the web page.
  6. ^ a b c d e f g Barstow, M. A.; Holberg, J. B.; Koester, D. (1994), "Extreme Ultraviolet Spectrophotometry of HD16538 and HR:8210 Ik-Pegasi", Monthly Notices of the Royal Astronomical Society, 270 (3): 516, Bibcode:1994MNRAS.270..516B, doi:10.1093/mnras/270.3.516
  7. ^ a b c d e f g h Wonnacott, D.; Kellett, B. J.; Smalley, B.; Lloyd, C. (1994), "Pulsational Activity on Ik-Pegasi", Monthly Notices of the Royal Astronomical Society, 267 (4): 1045–1052, Bibcode:1994MNRAS.267.1045W, doi:10.1093/mnras/267.4.1045
  8. ^ a b Smalley, B.; et al. (1996), "The chemical composition of IK Pegasi", Monthly Notices of the Royal Astronomical Society, 278 (3): 688–696, Bibcode:1996MNRAS.278..688S, doi:10.1093/mnras/278.3.688
  9. ^ a b c d e Landsman, W.; Simon, T.; Bergeron, P. (1999), "The hot white-dwarf companions of HR 1608, HR 8210, and HD 15638", Publications of the Astronomical Society of the Pacific, 105 (690): 841–847, Bibcode:1993PASP..105..841L, doi:10.1086/133242
  10. ^ a b Vennes, S.; Christian, D. J.; Thorstensen, J. R. (1998), "Hot White Dwarfs in the Extreme-Ultraviolet Explorer Survey. IV. DA White Dwarfs with Bright Companions", The Astrophysical Journal, 502 (2): 763–787, Bibcode:1998ApJ...502..763V, doi:10.1086/305926
  11. ^ Vallerga, John (1998), "The Stellar Extreme-Ultraviolet Radiation Field", Astrophysical Journal, 497 (2): 77–115, Bibcode:1998ApJ...497..921V, doi:10.1086/305496
  12. ^ Mazzali, P. A.; Röpke, F. K.; Benetti, S.; Hillebrandt, W. (2007). "A Common Explosion Mechanism for Type Ia Supernovae". Science (PDF). 315 (5813): 825–828. arXiv:astro-ph/0702351v1. Bibcode:2007Sci...315..825M. doi:10.1126/science.1136259. PMID 17289993. S2CID 16408991.
  13. ^ a b c d Wonnacott, D.; Kellett, B. J.; Stickland, D. J. (1993), "IK Peg - A nearby, short-period, Sirius-like system", Monthly Notices of the Royal Astronomical Society, 262 (2): 277–284, Bibcode:1993MNRAS.262..277W, doi:10.1093/mnras/262.2.277
  14. ^ Pickering, Edward Charles (1908), "Revised Harvard photometry: a catalogue of the positions, photometric magnitudes and spectra of 9110 stars, mainly of the magnitude 6.50, and brighter observed with the 2 and 4-inch (100 mm) meridian photometers", Annals of the Astronomical Observatory of Harvard College, 50: 182, Bibcode:1908AnHar..50....1P
  15. ^ Rabinowitz, Harold; Vogel, Suzanne (2009), The manual of scientific style: a guide for authors, editors, and researchers, Academic Press, p. 364, ISBN 978-0-12-373980-3
  16. ^ Staff, Spectroscopic Binaries, University of Tennessee, retrieved 2007-06-09
  17. ^ Harper, W. E. (1928), "The orbits of A Persei and HR 8210", Publications of the Dominion Astrophysical Observatory, 4: 161–169, Bibcode:1928PDAO....4..171H
  18. ^ Perryman, M. A. C.; et al. (1997), "The Hipparcos Catalogue", Astronomy & Astrophysics, 323: L49–L52, Bibcode:1997A&A...323L..49P
  19. ^ Wilson, Ralph Elmer (1953), "General catalogue of stellar radial velocities", Carnegie Institute Washington D.C. Publication, Carnegie Institution of Washington, Bibcode:1953GCRV..C......0W
  20. ^ Burleigh, M. R.; et al. (July 28 – August 1, 1975), "Resolving Sirius-like Binaries with the Hubble Space Telescope", in Provencal, J. L.; Shipman, H. L.; MacDonald, J.; Goodchild, S. (eds.), Proceedings 12th European Workshop on White Dwarfs, vol. 226, San Francisco: Astronomy Society of the Pacific, p. 222, arXiv:astro-ph/0010181, Bibcode:2001ASPC..226..222B, ISBN 1-58381-058-7
  21. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 30 November 2022.
  22. ^ a b Gautschy, A.; Saio, H. (1995), "Stellar Pulsations Across The HR Diagram: Part 1", Annual Review of Astronomy and Astrophysics, 33 (1): 75–114, Bibcode:1995ARA&A..33...75G, doi:10.1146/annurev.aa.33.090195.000451
  23. ^ For an explanation of the star colors, see: "The Colour of Stars". Australia Telescope Outreach and Education. December 21, 2004. Archived from the original on March 18, 2012. Retrieved 2007-09-26.
  24. ^ Templeton, Matthew (2004), Variable Star of the Season: Delta Scuti and the Delta Scuti variables, AAVSO, retrieved 2021-05-06
  25. ^ Saha, Swapan K. (2007), Diffraction-limited imaging with large and moderate telescopes, World Scientific, p. 440, Bibcode:2007dlil.book.....S, ISBN 978-981-270-777-2
  26. ^ Mayer, J. G.; Hakkila, J. (1994), "Photometric Effects of Binarity on AM Star Broadband Colors", Bulletin of the American Astronomical Society, 26: 868, Bibcode:1994AAS...184.0607M
  27. ^ Anonymous (2005), Stellar Lifetimes, Georgia State University, retrieved 2007-02-26
  28. ^ Staff (August 29, 2006), White Dwarfs & Planetary Nebulas, Harvard-Smithsonian Center for Astrophysics, retrieved 2007-06-09
  29. ^ Heger, A.; et al. (2003), "§3, How Massive Single Stars End Their Life", Astrophysical Journal, 591 (1): 288–300, arXiv:astro-ph/0212469, Bibcode:2003ApJ...591..288H, doi:10.1086/375341, S2CID 59065632
  30. ^ Seligman, Courtney (2007), The Mass-Luminosity Diagram and the Lifetime of Main-Sequence Stars, retrieved 2007-05-14
  31. ^ Staff (August 29, 2006), Stellar Evolution - Cycles of Formation and Destruction, Harvard-Smithsonian Center for Astrophysics, retrieved 2006-08-10
  32. ^ Richmond, Michael (October 5, 2006), Late stages of evolution for low-mass stars, Rochester Institute of Technology, retrieved 2007-06-07
  33. ^ Darling, David, Carbon burning, The Internet Encyclopedia of Science, retrieved 2007-08-15
  34. ^ Savage, D.; Jones, T.; Villard, Ray; Watzke, M. (August 6, 1997), Hubble Separates Stars in the Mira Binary System, HubbleSite News Center, retrieved 2007-03-01
  35. ^ Oberhummer, H.; Csótó, A.; Schlattl, H. (2000), "Stellar Production Rates of Carbon and Its Abundance in the Universe", Science, 289 (5476): 88–90, arXiv:astro-ph/0007178, Bibcode:2000Sci...289...88O, doi:10.1126/science.289.5476.88, PMID 10884230, S2CID 2884928
  36. ^ Iben, Icko Jr. (1991), "Single and binary star evolution", Astrophysical Journal Supplement Series, 76: 55–114, Bibcode:1991ApJS...76...55I, doi:10.1086/191565
  37. ^ Gil-Pons, P.; García-Berro, E. (2001), "On the formation of oxygen-neon white dwarfs in close binary systems", Astronomy and Astrophysics, 375 (1): 87–99, arXiv:astro-ph/0106224, Bibcode:2001A&A...375...87G, doi:10.1051/0004-6361:20010828, S2CID 11890376
  38. ^ Woosley, S. E.; Heger, A. (2002), "The Evolution and Explosion of Massive Stars" (PDF), Reviews of Modern Physics, 74 (4): 1015–1071, Bibcode:2002RvMP...74.1015W, doi:10.1103/RevModPhys.74.1015, retrieved 2021-05-06
  39. ^ Estimating Stellar Parameters from Energy Equipartition, ScienceBits, retrieved 2007-05-15
  40. ^ Imamura, James N. (February 24, 1995), Cooling of White Dwarfs, University of Oregon, archived from the original on May 2, 2007, retrieved 2007-05-19
  41. ^ Postnov, K. A.; Yungelson, L. R. (2006), "The Evolution of Compact Binary Star Systems", Living Reviews in Relativity, 9 (1): 6, arXiv:astro-ph/0701059, Bibcode:2006LRR.....9....6P, doi:10.12942/lrr-2006-6, PMC 5253975, PMID 28163653
  42. ^ Malatesta, K.; Davis, K. (May 2001), Variable Star Of The Month: A Historical Look at Novae (PDF), AAVSO, retrieved 2021-05-06
  43. ^ a b Malatesta, Kerri (May 2000), Variable Star Of The Month—May, 2000: RS Ophiuchi, AAVSO, retrieved 2021-05-06
  44. ^ Hendrix, Susan (July 20, 2007), Scientists see Storm Before the Storm in Future Supernova, NASA, retrieved 2007-05-25
  45. ^ Langer, N.; Deutschmann, A.; Wellstein, S.; Höflich, P. (2000), "The evolution of main sequence star + white dwarf binary systems towards Type Ia supernovae", Astronomy and Astrophysics, 362: 1046–1064, arXiv:astro-ph/0008444, Bibcode:2000A&A...362.1046L
  46. ^ Langer, N.; Yoon, S.-C.; Wellstein, S.; Scheithauer, S. (2002), "On the evolution of interacting binaries which contain a white dwarf", in Gänsicke, B. T.; Beuermann, K.; Rein, K. (eds.), The Physics of Cataclysmic Variables and Related Objects, ASP Conference Proceedings, vol. 261, San Francisco, California: Astronomical Society of the Pacific, p. 252, Bibcode:2002ASPC..261..252L
  47. ^ Di Stefano, Rosanne (February 28 – March 1, 1996), "Luminous Supersoft X-Ray Sources as Progenitors of Type Ia Supernovae", in J. Greiner (ed.), Proceedings of the International Workshop on Supersoft X-Ray Sources, Garching, Germany: Springer-Verlag, arXiv:astro-ph/9701199, Bibcode:1997astro.ph..1199D
  48. ^ Fryer, C. L.; New, K. C. B. (January 24, 2006), "2.1 Collapse scenario", Gravitational Waves from Gravitational Collapse, Max-Planck-Gesellschaft, archived from the original on March 27, 2011, retrieved 2007-06-07
  49. ^ Staff (August 29, 2006), Stellar Evolution - Cycles of Formation and Destruction, Harvard-Smithsonian Center for Astrophysics, retrieved 2006-08-10
  50. ^ a b Beech, Martin (2011), "The past, present and future supernova threat to Earth's biosphere", Astrophysics and Space Science, 336 (2), Springer: 287–302, Bibcode:2011Ap&SS.336..287B, doi:10.1007/s10509-011-0873-9, S2CID 119803426
  51. ^ Richmond, Michael (April 8, 2005), Will a Nearby Supernova Endanger Life on Earth?, archived from the original (TXT) on March 6, 2007, retrieved 2006-03-30—see section 4.
  52. ^ Hansen, Brad M. S. (2003), "Type Ia Supernovae and High-Velocity White Dwarfs", The Astrophysical Journal, 582 (2): 915–918, arXiv:astro-ph/0206152, Bibcode:2003ApJ...582..915H, doi:10.1086/344782, S2CID 16653531
  53. ^ Marietta, E.; Burrows, A.; Fryxell, B. (2000), "Type Ia Supernova Explosions in Binary Systems: The Impact on the Secondary Star and Its Consequences", The Astrophysical Journal Supplement Series, 128 (2): 615–650, arXiv:astro-ph/9908116, Bibcode:2000ApJS..128..615M, doi:10.1086/313392, S2CID 17251956
  54. ^ Staff (September 7, 2006), Introduction to Supernova Remnants, NASA/Goddard, retrieved 2007-05-20
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