List of white dwarfs

Last updated

This is a list of exceptional white dwarf stars.

Firsts

These were the first white dwarfs discovered fitting these conditions

Contents

TitleStarDateDataCommentsNotesRefs
First discovered Sirius B 1852 Sirius systemSirius B is also the nearest white dwarf (as of 2005) [1] [2]
First found in a binary star system
First double white dwarf system LDS 275 1944 L 462-56 system [3]
First solitary white dwarf Van Maanen 2 1917Van Maanen's star is also the nearest solitary white dwarf [4]
First white dwarf with a planet WD B1620−26 2003 PSR B1620-26 b (planet)This planet is a circumbinary planet, which circles both stars in the PSR B1620-26 system [5] [6]
First singular white dwarf with a planet WD 1145+017 2015 WD 1145+017 b Planet is extremely small and is disintegrating.
First white dwarf that is a pulsar AR Scorpii A 2016The star is in a binary system with a red dwarf [7]

Extremes

These are the white dwarfs which are currently known to fit these conditions

TitleStarDateDataCommentsNotesRefs
NearestSirius18528.6  ly (2.6  pc )Sirius B is also the second white dwarf discovered. [1] [2]
Farthest SN UDS10Wil progenitor 201310,000,000,000 ly z=1.914 SN Wilson is a type-Ia supernova whose progenitor was a white dwarf [8] [9] [10]
Oldest WD 0346+246 202111.5 billion years [11]
Youngestprovisional estimate
Highest surface temperature RX J0439.8−6809 2015250,000  K (250,000  °C ; 450,000  °F )This star is located in the Milky Way's galactic halo, in the field of the Large Magellanic Cloud [12] [13] [11]
Lowest surface temperature PSR J2222–0137 B20213,000  K (2,730  °C ; 4,940  °F ) [11]
Most luminous Z Andromedae B1,500 - 9,800 L☉ [14]
Least luminous2014
Brightest apparentSirius B18528.44 (V)
Dimmest apparent
Most massive ZTF J1901+1458 [15] 20201.35 M☉ [15]
Least massive NLTT 11748 20070.13–0.16 M☉ [11]
Largest Z Andromedae B0.17—0.16 R☉ [16]
Smallest HD 49798 20210.0023  R☉ [17]

Nearest

10 nearest white dwarfs
StarDistanceCommentsNotesRefs
Sirius B 8.58 ly (2.63 pc)Sirius B is also the second white dwarf discovered. It is part of the Sirius system. [1] [2] [18] [19]
Procyon B 11.43 ly (3.50 pc)Part of Procyon system [18] [19]
van Maanen's Star 14.04 ly (4.30 pc) [18] [19]
GJ 440 15.09 ly (4.63 pc) [18]
40 Eridani B 16.25 ly (4.98 pc)Part of 40 Eridani system [18] [19]
Stein 2051 B 18.06 ly (5.54 pc)Part of Stein 2051 system [18] [19]
LP 44-113 20.0 ly (6.1 pc) [19]
G 99-44 20.9 ly (6.4 pc) [19]
L 97-12 25.8 ly (7.9 pc) [19]
Wolf 489 26.7 ly (8.2 pc) [19]

Other notable white dwarfs

    Related Research Articles

    <span class="mw-page-title-main">Supernova</span> Explosion of a star at its end of life

    A supernova is a powerful and luminous explosion of a star. A supernova occurs during the last evolutionary stages of a massive star, or when a white dwarf is triggered into runaway nuclear fusion. The original object, called the progenitor, either collapses to a neutron star or black hole, or is completely destroyed to form a diffuse nebula. The peak optical luminosity of a supernova can be comparable to that of an entire galaxy before fading over several weeks or months.

    <span class="mw-page-title-main">Superluminous supernova</span> Supernova at least ten times more luminous than a standard supernova

    A super-luminous supernova is a type of stellar explosion with a luminosity 10 or more times higher than that of standard supernovae. Like supernovae, SLSNe seem to be produced by several mechanisms, which is readily revealed by their light-curves and spectra. There are multiple models for what conditions may produce an SLSN, including core collapse in particularly massive stars, millisecond magnetars, interaction with circumstellar material, or pair-instability supernovae.

    <span class="mw-page-title-main">Blue supergiant</span> Hot, luminous star with a spectral type of B9 (or A9) or earlier

    A blue supergiant (BSG) is a hot, luminous star, often referred to as an OB supergiant. They are usually considered to be those with luminosity class I and spectral class B9 or earlier, although sometimes A-class supergiants are also deemed blue supergiants.

    <span class="mw-page-title-main">Luminous blue variable</span> Type of star that is luminous, blue, and variable in brightness

    Luminous blue variables (LBVs) are massive evolved stars that show unpredictable and sometimes dramatic variations in their spectra and brightness. They are also known as S Doradus variables after S Doradus, one of the brightest stars of the Large Magellanic Cloud. They are considered to be rare.

    <span class="mw-page-title-main">Delta Andromedae</span> Multiple star system in the constellation Andromeda

    Delta Andromedae, Latinized from δ Andromedae, is a triple star system in the northern constellation of Andromeda. The system is visible to the naked eye as a point of light with a combined apparent visual magnitude of 3.28. Based upon parallax measurements, it is located at a distance of approximately 105.5 light-years from the Sun. The system is drifting closer with a radial velocity of −10 km/s.

    11 Andromedae, abbreviated 11 And, is a single, orange-hued star in the northern constellation of Andromeda. 11 Andromedae is the Flamsteed designation. It has an apparent visual magnitude of 5.44, which is bright enough to be faintly visible to the naked eye. An annual parallax shift of 11.5 mas yields a distance estimate of 283 light years. It is moving further from the Earth with a heliocentric radial velocity of +10 km/s.

    <span class="mw-page-title-main">Gliese 687</span> Star in the constellation Draco

    Gliese 687, or GJ 687 (Gliese–Jahreiß 687) is a red dwarf in the constellation Draco. This is one of the closest stars to the Sun and lies at an approximate distance of less than 15 light years. Even though it is close by, it has a magnitude of about 9, so it can only be seen through a moderately sized telescope. Gliese 687 has a high proper motion, advancing 1.304 arcseconds per year across the sky. It has a net relative velocity of about 39 km/s. It is known to have a Neptune-mass planet. Old books and articles refer to it as Argelander Oeltzen 17415.

    The Hungarian Automated Telescope Network (HATNet) project is a network of six small fully automated "HAT" telescopes. The scientific goal of the project is to detect and characterize extrasolar planets using the transit method. This network is used also to find and follow bright variable stars. The network is maintained by the Center for Astrophysics | Harvard & Smithsonian.

    Z Andromedae is a binary star system consisting of a red giant and a white dwarf. It is the prototype of a type of cataclysmic variable star known as symbiotic variable stars or simply Z Andromedae variables. The brightness of those stars vary over time, showing a quiescent, more stable phase and then an active one with a more pronounced variability and stronger brightening and/or dimming.

    A pulsating white dwarf is a white dwarf star whose luminosity varies due to non-radial gravity wave pulsations within itself. Known types of pulsating white dwarfs include DAV, or ZZ Ceti, stars, with hydrogen-dominated atmospheres and the spectral type DA; DBV, or V777 Her, stars, with helium-dominated atmospheres and the spectral type DB; and GW Vir stars, with atmospheres dominated by helium, carbon, and oxygen, and the spectral type PG 1159. GW Vir stars may be subdivided into DOV and PNNV stars; they are not, strictly speaking, white dwarfs but pre-white dwarfs which have not yet reached the white dwarf region on the Hertzsprung-Russell diagram. A subtype of DQV stars, with carbon-dominated atmospheres, has also been proposed, and in May 2012, the first extremely low mass variable (ELMV) white dwarf was reported.

    <span class="mw-page-title-main">Tycho G</span> Star in the constellation Cassiopeia

    Tycho G has been proposed as the surviving binary companion star of the SN 1572 supernova event. The star is located about 6,400±1,500 light-years away in the constellation Cassiopeia. It is a subgiant, similar to the Sun in temperature, but more evolved and luminous.

    <span class="mw-page-title-main">RX Andromedae</span> Cataclysmic variable star system in the constellation Andromeda

    RX Andromedae is a variable star in the constellation of Andromeda. Although it is classified as a dwarf nova of the Z Camelopardalis (UGZ) type, it has shown low-luminosity periods typical of VY Sculptoris stars. However, for most of the time it varies from an apparent visual magnitude of 15.1 at minimum brightness to a magnitude of 10.2 at maximum brightness, with a period of approximately 13 days.

    In astronomy, a calcium-rich supernova is a subclass of supernovae that, in contrast to more well-known traditional supernova classes, are fainter and produce unusually large amounts of calcium. Since their luminosity is located in a gap between that of novae and other supernovae, they are also referred to as "gap" transients. Only around 15 events have been classified as a calcium-rich supernova – a combination of their intrinsic rarity and low luminosity make new discoveries and their subsequent study difficult. This makes calcium-rich supernovae one of the most mysterious supernova subclasses currently known.

    SN 2009ip was a supernova discovered in 2009 in the spiral galaxy NGC 7259 in the constellation of Piscis Austrinus. Since the brightness waned after days post-discovery, it was redesignated as Luminous blue variable (LBV) Supernova impostor.

    <span class="mw-page-title-main">EG Andromedae</span> Binary star system in the constellation Andromeda

    EG Andromedae is a symbiotic binary in the constellation Andromeda. Its apparent visual magnitude varies between 6.97 and 7.80.

    <span class="mw-page-title-main">V455 Andromedae</span> Dwarf nova star in the constellation Andromeda

    V455 Andromedae is a dwarf nova in the constellation Andromeda. It has a typical apparent visual magnitude of 16.5, but reached a magnitude of 8.5 during the only observed outburst.

    <span class="mw-page-title-main">NGC 4636</span> Galaxy in the constellation Virgo

    NGC 4636 is an elliptical galaxy located in the constellation Virgo. It is a member of the NGC 4753 Group of galaxies, which is a member of the Virgo II Groups, a series of galaxies and galaxy clusters strung out from the southern edge of the Virgo Supercluster. It is located at a distance of about 55 million light years from Earth, which, given its apparent dimensions, means that NGC 4636 is about 105,000 light years across.

    References

    1. 1 2 3 Atlas of the Universe, "The Universe within 12.5 Light Years: The Nearest Stars", Richard Powell, 30 July 2006 (accessed 2010-11-01)
    2. 1 2 3 BBC News, "Hubble finds mass of white dwarf", Christine McGourty, 14 December 2005 (accessed 2010-11-01)
    3. ↑ W. J. Luyten (September 1944). "Note on the Double White Dwarf L 462-56 = LDS 275". Astrophysical Journal. 100: 202. Bibcode:1944ApJ...100..202L. doi:10.1086/144658.
    4. ↑ Schatzman, Évry (1958), White Dwarfs, North Holland Publishing Company, p. 2.
    5. ↑ Steinn Sigurdsson; Harvey B. Richer; Brad M. Hansen; Ingrid H. Stairs; Stephen E. Thorsett (July 2003). "A Young White Dwarf Companion to Pulsar B1620-26: Evidence for Early Planet Formation". Science. 301 (5630): 193–196. arXiv: astro-ph/0307339 . Bibcode:2003Sci...301..193S. doi:10.1126/science.1086326. PMID   12855802. S2CID   39446560.
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    7. ↑ Hambsch, Franz-Josef. "Amateurs Help Discover Pulsing White Dwarf". Sky and Telescope.
    8. ↑ Jason Major (5 April 2013). "Hubble Spots the Most Distant Supernova Ever". Discovery Channel.
    9. ↑ "CANDELS Finds the Most Distant Type Ia Supernova Yet Observed". Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS). 23 April 2013.
    10. ↑ David O. Jones; Steven A. Rodney; Adam G. Riess; Bahram Mobasher; Tomas Dahlen; Curtis McCully; Teddy F. Frederiksen; Stefano Casertano; Jens Hjorth; Charles R. Keeton; Anton Koekemoer; Louis-Gregory Strolger; Tommy G. Wiklind; Peter Challis; Or Graur; Brian Hayden; Brandon Patel; Benjamin J. Weiner; Alexei V. Filippenko; Peter Garnavich; Saurabh W. Jha; Robert P. Kirshner; Henry C. Ferguson; Norman A. Grogin; Dale Kocevski (2 April 2013). "The Discovery of the Most Distant Known Type Ia Supernova at Redshift 1.914". The Astrophysical Journal. 768 (2) (published May 2013): 166. arXiv: 1304.0768 . Bibcode:2013ApJ...768..166J. doi:10.1088/0004-637X/768/2/166. S2CID   118890248. 166.
    11. 1 2 3 4 Lacki, Brian C.; Brzycki, Bryan; Croft, Steve; Czech, Daniel; DeBoer, David; DeMarines, Julia; Gajjar, Vishal; Isaacson, Howard; Lebofsky, Matt; MacMahon, David H. E.; Price, Danny C.; Sheikh, Sofia Z.; Siemion, Andrew P. V.; Drew, Jamie; Worden, S. Pete (2021-11-24). "One of Everything: The Breakthrough Listen Exotica Catalog". The Astrophysical Journal Supplement Series. 257 (2): 42. arXiv: 2006.11304 . Bibcode:2021ApJS..257...42L. doi: 10.3847/1538-4365/ac168a . ISSN   0067-0049.
    12. ↑ Universitaet Tübingen (24 November 2015). "The hottest white dwarf in the Galaxy". Science Daily.
    13. ↑ K. Werner; T. Rauch (29 September 2015). "Analysis of HST/COS spectra of the bare C–O stellar core H1504+65 and a high-velocity twin in the Galactic halo". Astronomy and Astrophysics. 584 (published December 2015): A19. arXiv: 1509.08942 . Bibcode:2015A&A...584A..19W. doi:10.1051/0004-6361/201527261. S2CID   118458007. A19.
    14. ↑ Sokoloski, J. L.; Kenyon, S. J.; Espey, B. R.; Keyes, Charles D.; McCandliss, S. R.; Kong, A. K. H.; Aufdenberg, J. P.; Filippenko, A. V.; Li, W.; Brocksopp, C.; Kaiser, Christian R.; Charles, P. A.; Rupen, M. P.; Stone, R. P. S. (2006-01-10). "A "Combination Nova" Outburst in Z Andromedae: Nuclear Shell Burning Triggered by a Disk Instability". The Astrophysical Journal. 636 (2): 1002–1019. arXiv: astro-ph/0509638 . Bibcode:2006ApJ...636.1002S. doi:10.1086/498206. ISSN   0004-637X. S2CID   8941207.
    15. 1 2 "A White Dwarf Living on the Edge". California Institute of Technology. 2021-06-30. Retrieved 2023-07-20.
    16. ↑ Sokoloski, J. L.; Kenyon, S. J.; Espey, B. R.; Keyes, Charles D.; McCandliss, S. R.; Kong, A. K. H.; Aufdenberg, J. P.; Filippenko, A. V.; Li, W.; Brocksopp, C.; Kaiser, Christian R.; Charles, P. A.; Rupen, M. P.; Stone, R. P. S. (2006-01-01). "A Combination Nova Outburst in Z Andromedae: Nuclear Shell Burning Triggered by a Disk Instability". The Astrophysical Journal. 636 (2): 1002–1019. arXiv: astro-ph/0509638 . Bibcode:2006ApJ...636.1002S. doi:10.1086/498206. ISSN   0004-637X.
    17. ↑ "New X-ray observations of the hot subdwarf binary HD 49798/RX J0648.0–4418". academic.oup.com. Retrieved 2023-01-08.
    18. 1 2 3 4 5 6 David Taylor (2012). "White Dwarf Stars Near The Earth" (PDF). The Life and Death of Stars. Weinberg College of Arts and Sciences - Northwestern University.
    19. 1 2 3 4 5 6 7 8 9 "White dwarfs within 10 parsecs". Sol Station. 2011.
    20. ↑ Caiazzo, Ilaria; Burdge, Kevin B.; Tremblay, Pier-Emmanuel; Fuller, James; Ferrario, Lilia; Gänsicke, Boris T.; Hermes, J. J.; Heyl, Jeremy; Kawka, Adela; Kulkarni, S. R.; Marsh, Thomas R.; Mróz, Przemek; Prince, Thomas A.; Richer, Harvey B.; Rodriguez, Antonio C. (2023-07-19). "A rotating white dwarf shows different compositions on its opposite faces". Nature. 620 (7972): 61–66. arXiv: 2308.07430 . Bibcode:2023Natur.620...61C. doi:10.1038/s41586-023-06171-9. ISSN   1476-4687.
    21. ↑ "Two-Faced Star Exposed". California Institute of Technology. 2023-07-19. Retrieved 2023-07-31.

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