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Super soft X-ray source

February 19, 2024

A luminous supersoft X-ray source (SSXS, or SSS) is an astronomical source that emits only low energy (i.e., soft) X-rays. Soft X-rays have energies in the 0.09 to 2.5 keV range, whereas hard X-rays are in the 1–20 keV range.[1] SSSs emit few or no photons with energies above 1 keV, and most have effective temperature below 100 eV. This means that the radiation they emit is highly ionizing and is readily absorbed by the interstellar medium. Most SSSs within our own galaxy are hidden by interstellar absorption in the galactic disk.[2] They are readily evident in external galaxies, with ~10 found in the Magellanic Clouds and at least 15 seen in M31.[2]

As of early 2005, more than 100 SSSs have been reported in ~20 external galaxies, the Large Magellanic Cloud (LMC), Small Magellanic Cloud (SMC), and the Milky Way (MW).[3] Those with luminosities below ~3 x 1038 erg/s are consistent with steady nuclear burning in accreting white dwarfs (WD)s or post-novae.[3] There are a few SSS with luminosities ≥1039 erg/s.[3]

Super soft X-rays are believed to be produced by steady nuclear fusion on a white dwarf's surface of material pulled from a binary companion,[4] the so-called close-binary supersoft source (CBSS).[5] This requires a flow of material sufficiently high to sustain the fusion. Contrast this with the nova, where less flow causes the material to only fuse sporadically. Super soft X-ray sources can evolve into type Ia supernova, where a sudden fusion of material destroys the white dwarf, and neutron stars, through collapse.[6]

Super soft X-ray sources were first discovered by the Einstein Observatory. Further discoveries were made by ROSAT.[7] Many different classes of objects emit supersoft X-radiation (emission dominantly below 0.5 keV).[5]

Luminous supersoft X-ray sources edit

Luminous super soft X-ray sources have a characteristic blackbody temperature of a few tens of eV (~20–100 eV)[3] and a bolometric luminosity of ~1038 erg/s (below ~ 3 x 1038 erg/s).[2][3]

Apparently, luminous SSXSs can have equivalent blackbody temperatures as low as ~15 eV and luminosities ranging from 1036 to 1038 erg/s.[8] The numbers of luminous SSSs in the disks of ordinary spiral galaxies such as the MW and M31 are estimated to be on the order of 103.[8]

Milky Way SSXSs edit

SSXSs have now been discovered in our galaxy and in globular cluster M3.[2] MR Velorum (RX J0925.7-4758) is one of the rare MW super soft X-ray binaries.[5] "The source is heavily reddened by interstellar material, making it difficult to observe in the blue and ultraviolet."[9] The period determined for MR Velorum at ~4.03 d is considerably longer than that of other supersoft systems, which is usually less than a day.[9]

Close-binary supersoft source (CBSS) edit

The CBSS model invokes steady nuclear burning on the surface of an accreting white dwarf (WD) as the generator of the prodigious super soft X-ray flux.[5] As of 1999, eight SSXSs have orbital periods between ~4 hr and 1.35 d: RX J0019.8+2156 (MW), RX J0439.8-6809 (MW halo near LMC), RX J0513.9-6951 (LMC), RX J0527.8-6954 (LMC), RX J0537.7-7034 (LMC), CAL 83 (LMC), CAL 87 LMC), and 1E 0035.4-7230 (SMC).[5]

Symbiotic binary edit

Main article: Symbiotic variable star

A symbiotic binary star is a variable binary star system in which a red giant has expanded its outer envelope and is shedding mass quickly, and another hot star (often a white dwarf) is ionizing the gas.[10] Three symbiotic binaries as of 1999 are SSXSs: AG Dra (BB, MW), RR Tel (WD, MW), and RX J0048.4-7332 (WD, SMC).[5]

Noninteracting white dwarfs edit

The youngest, hottest WD, KPD 0005+5106, is very close to 100,000 K, of type DO and is the first single WD recorded as an X-ray source with ROSAT.[11][12]

Cataclysmic variables edit

Main article: Cataclysmic variable star

"Cataclysmic variables (CVs) are close binary systems consisting of a white dwarf and a red-dwarf secondary transferring matter via the Roche lobe overflow."[13] Both fusion- and accretion-powered cataclysmic variables have been observed to be X-ray sources.[14] The accretion disk may be prone to instability leading to dwarf nova outbursts: a portion of the disk material falls onto the white dwarf, the cataclysmic outbursts occur when the density and temperature at the bottom of the accumulated hydrogen layer rise high enough to ignite nuclear fusion reactions, which rapidly burn the hydrogen layer to helium.

Apparently the only SSXS nonmagnetic cataclysmic variable is V Sagittae: bolometric luminosity of (1–10) x 1037, a binary including a blackbody (BB) accretor at T < 80 eV, and an orbital period of 0.514195 d.[5]

The accretion disk can become thermally stable in systems with high mass-transfer rates (Ṁ).[13] Such systems are called nova-like (NL) stars, because they lack outbursts characteristic of dwarf novae.[15]

VY Scl cataclysmic variables edit

Among the NL stars is a small group which shows a temporary reduction or cessation of Ṁ from the secondary. These are the VY Scl-type stars or anti-dwarf novae.[16]

V751 Cyg edit

V751 Cyg (BB, MW) is a VY Scl CV, has a bolometric luminosity of 6.5 x 1036 erg/s,[5] and emits soft X-rays at quiescence.[17] The discovery of a weak soft X-ray source of V751 Cyg at minimum presents a challenge as this is unusual for CVs which commonly display weak hard X-ray emission at quiescence.[17]

The high luminosity (6.5 x 1036 erg/s) is particularly hard to understand in the context of VY Scl stars generally, because observations suggest that the binaries become simple red dwarf + white dwarf pairs at quiescence (the disk mostly disappears).[17] "A high luminosity in soft X-rays poses an additional problem of understanding why the spectrum is of only modest excitation."[17] The ratio He II λ4686/Hβ did not exceed ~0.5 in any of the spectra recorded up to 2001, which is typical for accretion-powered CVs and does not approach the ratio of 2 commonly seen in supersoft binaries (CBSS).[17]

Pushing the edge of acceptable X-ray fits toward lower luminosity suggests that the luminosity should not exceed ~2 x 1033 ergs/s, which gives only ~4 x 1031 ergs/s of reprocessed light in the WD about equal to the secondary's expected nuclear luminosity.[17]

Magnetic cataclysmic variables edit

Main article: Polar (cataclysmic variable)

X-rays from magnetic cataclysmic variables are common because accretion provides a continuous supply of coronal gas.[18] A plot of number of systems vs. orbit period shows a statistically significant minimum for periods between 2 and 3 hr which can probably be understood in terms of the effects of magnetic braking when the companion star becomes completely convective and the usual dynamo (which operates at the base of the convective envelope) can no longer give the companion a magnetic wind to carry off angular momentum.[18] The rotation has been blamed on asymmetric ejection of planetary nebulae and winds[19] and the fields on in situ dynamos.[20] Orbit and rotation periods are synchronized in strongly magnetized WDs.[18] Those with no detectable field never are synchronized.

With temperatures in the range 11,000 to 15,000 K, all the WDs with the most extreme fields are far too cool to be detectable EUV/X-ray sources, e.g., Grw +70°8247, LB 11146, SBS 1349+5434, PG 1031+234 and GD 229.[21]

Most highly magnetic WDs appear to be isolated objects, although G 23–46 (7.4 MG) and LB 1116 (670 MG) are in unresolved binary systems.[22]

RE J0317-853 is the hottest magnetic WD at 49,250 K, with an exceptionally intense magnetic field of ~340 MG, and implied rotation period of 725.4 s.[22] Between 0.1 and 0.4 keV, RE J0317-853 was detectable by ROSAT, but not in the higher energy band from 0.4 to 2.4 keV.[citation needed] RE J0317-853 is associated with a blue star 16 arcsec from LB 9802 (also a blue WD) but not physically associated.[22] A centered dipole field is not able to reproduce the observations, but an off-center dipole 664 MG at the south pole and 197 MG at the north pole does.[22]

Until recently (1995) only PG 1658+441 possessed an effective temperature > 30,000 K.[22] Its polar field strength is only 3 MG.[22]

The ROSAT Wide Field Camera (WFC) source RE J0616-649 has an ~20 MG field.[23]

PG 1031+234 has a surface field that spans the range from ~200 MG to nearly 1000 MG and rotates with a period of 3h24m.[24]

The magnetic fields in CVs are confined to a narrow range of strengths, with a maximum of 7080 MG for RX J1938.4-4623.[25]

None of the single magnetic stars has been seen as of 1999 as an X-ray source, although fields are of direct relevance to the maintenance of coronae in main sequence stars.[18]

PG 1159 stars edit

PG 1159 stars are a group of very hot, often pulsating WDs for which the prototype is PG 1159 dominated by carbon and oxygen in their atmospheres.[18]

PG 1159 stars reach luminosities of ~1038 erg/s but form a rather distinct class.[26] RX J0122.9-7521 has been identified as a galactic PG 1159 star.[27][28]

Nova edit

Main article: Nova

There are three SSXSs with bolometric luminosity of ~1038 erg/s that are novae: GQ Mus (BB, MW), V1974 Cyg (WD, MW), and Nova LMC 1995 (WD).[5] Apparently, as of 1999 the orbital period of Nova LMC 1995 if a binary was not known.

U Sco, a recurrent nova as of 1999 unobserved by ROSAT, is a WD (74–76 eV), Lbol ~ (8–60) x 1036 erg/s, with an orbital period of 1.2306 d.[5]

Planetary nebula edit

Main article: Planetary nebula

In the SMC, 1E 0056.8-7154 is a WD with bolometric luminosity of 2 x 1037 that has a planetary nebula associated with it.[5]

Super soft active galactic nuclei edit

Supersoft active galactic nuclei reach luminosities up to 1045 erg/s.[5]

Large amplitude outbursts edit

Large amplitude outbursts of super soft X-ray emission have been interpreted as tidal disruption events.[29]

See also edit

References edit

  1. ^ . Archived from the original on 2008-06-07.
  2. ^ a b c d White NE; Giommi P; Heise J; Angelini L; et al. (1995). . The Astrophysical Journal. 445: L125. Bibcode:1995ApJ...445L.125W. doi:10.1086/187905. Archived from the original on 2009-07-03.
  3. ^ a b c d e Kahabka P (Dec 2006). "Supersoft X-ray sources". Advances in Space Research. 38 (12): 2836–9. Bibcode:2006AdSpR..38.2836K. doi:10.1016/j.asr.2005.10.058.
  4. ^ Max Planck Institute for Extraterrestrial Physics. "Super Soft X-ray Sources - Discovered with ROSAT".
  5. ^ a b c d e f g h i j k l Greiner J (2000). "Catalog of supersoft X-ray sources". New Astronomy. 5 (3): 137–41. arXiv:astro-ph/0005238. Bibcode:2000NewA....5..137G. doi:10.1016/S1384-1076(00)00018-X. S2CID 52241439.
  6. ^ Max Planck Institute for Extraterrestrial Physics. "Proceedings of the Workshop on Supersoft X-ray Sources".
  7. ^ . Archived from the original on 2007-11-28.
  8. ^ a b Kahabka P; van den Heuvel EPJ (1997). "Luminous Supersoft X-Ray Sources" (PDF). Annual Review of Astronomy and Astrophysics. 35 (1): 69–100. Bibcode:1997ARA&A..35...69K. doi:10.1146/annurev.astro.35.1.69. S2CID 70774203.
  9. ^ a b Schmidtke PC; Cowley AP (Sep 2001). "Synoptic Observations of the Supersoft Binary MR Velorum (RX J0925.7-4758): Determination of the Orbital Period". The Astronomical Journal. 122 (3): 1569–71. Bibcode:2001AJ....122.1569S. doi:10.1086/322155.
  10. ^ "David Darling site symbiotic star description".
  11. ^ Fleming TA; Werner K; Barstow MA (October 1993). "Detection of the First Coronal X-Ray Source about a White Dwarf". The Astrophysical Journal. 416: L79. Bibcode:1993ApJ...416L..79F. doi:10.1086/187075.
  12. ^ Werner (1994). "Spectral analysis of the hottest known helium-rich white dwarf: KPD 0005+5106". Astronomy and Astrophysics. 284: 907. Bibcode:1994A&A...284..907W.
  13. ^ a b Kato T; Ishioka R; Uemura M (Dec 2002). "Photometric Study of KR Aurigae during the High State in 2001". Publications of the Astronomical Society of Japan. 54 (6): 1033–9. arXiv:astro-ph/0209351. Bibcode:2002PASJ...54.1033K. doi:10.1093/pasj/54.6.1033.
  14. ^ "Introduction to Cataclysmic Variables (CVs)".
  15. ^ Osaki, Yoji (1996). "Dwarf-Nova Outbursts". Publications of the Astronomical Society of the Pacific. 108: 39. Bibcode:1996PASP..108...39O. doi:10.1086/133689.
  16. ^ Warner B (1995). Cataclysmic Variable Stars. Cambridge: Cambridge University Press. Bibcode:1995cvs..book.....W.
  17. ^ a b c d e f Patterson J; Thorstensen JR; Fried R; Skillman DR; et al. (Jan 2001). "Superhumps in Cataclysmic Binaries. XX. V751 Cygni". Publications of the Astronomical Society of the Pacific. 113 (779): 72–81. Bibcode:2001PASP..113...72P. doi:10.1086/317973.
  18. ^ a b c d e Trimble V (1999). "White dwarfs in the 1990s". Bulletin of the Astronomical Society of India. 27: 549–66. Bibcode:1999BASI...27..549T.
  19. ^ Spruit HC (1998). "Origin of the rotation rates of single white dwarfs". Astronomy and Astrophysics. 333: 603. arXiv:astro-ph/9802141. Bibcode:1998A&A...333..603S.
  20. ^ Schmidt GD; Grauer AD (1997). "Upper Limits for Magnetic Fields on Pulsating White Dwarfs". The Astrophysical Journal. 488 (2): 827–830. Bibcode:1997ApJ...488..827S. doi:10.1086/304746.
  21. ^ Schmidt GD; Smith PS (1995). "A Search for Magnetic Fields among DA White Dwarfs". The Astrophysical Journal. 448: 305. Bibcode:1995ApJ...448..305S. doi:10.1086/175962.
  22. ^ a b c d e f Barstow MA; Jordan S; O'Donoghue D; Burleigh MR; et al. (1995). "RE J0317-853: the hottest known highly magnetic DA white dwarf". Monthly Notices of the Royal Astronomical Society. 277 (3): 931–85. Bibcode:1995MNRAS.277..971B. doi:10.1093/mnras/277.3.971.
  23. ^ Barstow, M. A.; Jordan, S.; O'Donoghue, D.; Burleigh, M. R.; et al. (December 1995). "RE J0317-853: the hottest known highly magnetic DA white dwarf". Monthly Notices of the Royal Astronomical Society. 277 (3): 971–985. Bibcode:1995MNRAS.277..971B. doi:10.1093/mnras/277.3.971.
  24. ^ Latter WB; Schmidt GD; Green RF (1987). "The rotationally modulated Zeeman spectrum at nearly 10 to the 9th Gauss of the white dwarf PG 1031 + 234". The Astrophysical Journal. 320: 308. Bibcode:1987ApJ...320..308L. doi:10.1086/165543.
  25. ^ Schwope AD; et al. (1995). "Two-pole accretion in the high-field polar RXJ 1938.6-4612". Astronomy and Astrophysics. 293: 764. Bibcode:1995A&A...293..764S.
  26. ^ Dreizler S; Werner K; Heber U (1995). "PG 1159 stars and their evolutionary link to DO white dwarfs". In Kӧster D; Werner K (eds.). White Dwarfs. Lecture Notes in Physics. Vol. 443. Berlin: Springer. pp. 160–170. doi:10.1007/3-540-59157-5_199. ISBN 978-3-540-59157-3.
  27. ^ Cowley AP; Schmidtke PC; Hutchings JB; Crampton D (1995). "X-Ray Discovery of a Hot PG1159 Star, RX J0122.9-7521". Publ. Astron. Soc. Pac. 107: 927. Bibcode:1995PASP..107..927C. doi:10.1086/133640.
  28. ^ Werner K; Wolff B; Cowley AP; Schmidtke PC; et al. (1996). "Non-LTE model atmosphere analysis of the supersoft X-ray source RX J0122.9-7521". In Greiner (ed.). Supersoft X-Ray Sources. Lecture Notes in Physics. Vol. 472. pp. 131–138. doi:10.1007/BFb0102256. ISBN 978-3-540-61390-9.
  29. ^ Komossa S; Greiner J (1999). "Discovery of a giant and luminous X-ray outburst from the optically inactive galaxy pair RX J1242.6-1119". Astron. Astrophys. 349: L45. arXiv:astro-ph/9908216. Bibcode:1999A&A...349L..45K.

February 19, 2024
super, soft, source, luminous, supersoft, source, ssxs, astronomical, source, that, emits, only, energy, soft, rays, soft, rays, have, energies, range, whereas, hard, rays, range, ssss, emit, photons, with, energies, above, most, have, effective, temperature, . A luminous supersoft X ray source SSXS or SSS is an astronomical source that emits only low energy i e soft X rays Soft X rays have energies in the 0 09 to 2 5 keV range whereas hard X rays are in the 1 20 keV range 1 SSSs emit few or no photons with energies above 1 keV and most have effective temperature below 100 eV This means that the radiation they emit is highly ionizing and is readily absorbed by the interstellar medium Most SSSs within our own galaxy are hidden by interstellar absorption in the galactic disk 2 They are readily evident in external galaxies with 10 found in the Magellanic Clouds and at least 15 seen in M31 2 As of early 2005 more than 100 SSSs have been reported in 20 external galaxies the Large Magellanic Cloud LMC Small Magellanic Cloud SMC and the Milky Way MW 3 Those with luminosities below 3 x 1038 erg s are consistent with steady nuclear burning in accreting white dwarfs WD s or post novae 3 There are a few SSS with luminosities 1039 erg s 3 Super soft X rays are believed to be produced by steady nuclear fusion on a white dwarf s surface of material pulled from a binary companion 4 the so called close binary supersoft source CBSS 5 This requires a flow of material sufficiently high to sustain the fusion Contrast this with the nova where less flow causes the material to only fuse sporadically Super soft X ray sources can evolve into type Ia supernova where a sudden fusion of material destroys the white dwarf and neutron stars through collapse 6 Super soft X ray sources were first discovered by the Einstein Observatory Further discoveries were made by ROSAT 7 Many different classes of objects emit supersoft X radiation emission dominantly below 0 5 keV 5 Contents 1 Luminous supersoft X ray sources 2 Milky Way SSXSs 3 Close binary supersoft source CBSS 4 Symbiotic binary 5 Noninteracting white dwarfs 6 Cataclysmic variables 7 VY Scl cataclysmic variables 7 1 V751 Cyg 8 Magnetic cataclysmic variables 9 PG 1159 stars 10 Nova 11 Planetary nebula 12 Super soft active galactic nuclei 13 Large amplitude outbursts 14 See also 15 ReferencesLuminous supersoft X ray sources editLuminous super soft X ray sources have a characteristic blackbody temperature of a few tens of eV 20 100 eV 3 and a bolometric luminosity of 1038 erg s below 3 x 1038 erg s 2 3 Apparently luminous SSXSs can have equivalent blackbody temperatures as low as 15 eV and luminosities ranging from 1036 to 1038 erg s 8 The numbers of luminous SSSs in the disks of ordinary spiral galaxies such as the MW and M31 are estimated to be on the order of 103 8 Milky Way SSXSs editSSXSs have now been discovered in our galaxy and in globular cluster M3 2 MR Velorum RX J0925 7 4758 is one of the rare MW super soft X ray binaries 5 The source is heavily reddened by interstellar material making it difficult to observe in the blue and ultraviolet 9 The period determined for MR Velorum at 4 03 d is considerably longer than that of other supersoft systems which is usually less than a day 9 Close binary supersoft source CBSS editThe CBSS model invokes steady nuclear burning on the surface of an accreting white dwarf WD as the generator of the prodigious super soft X ray flux 5 As of 1999 eight SSXSs have orbital periods between 4 hr and 1 35 d RX J0019 8 2156 MW RX J0439 8 6809 MW halo near LMC RX J0513 9 6951 LMC RX J0527 8 6954 LMC RX J0537 7 7034 LMC CAL 83 LMC CAL 87 LMC and 1E 0035 4 7230 SMC 5 Symbiotic binary editMain article Symbiotic variable star A symbiotic binary star is a variable binary star system in which a red giant has expanded its outer envelope and is shedding mass quickly and another hot star often a white dwarf is ionizing the gas 10 Three symbiotic binaries as of 1999 are SSXSs AG Dra BB MW RR Tel WD MW and RX J0048 4 7332 WD SMC 5 Noninteracting white dwarfs editThe youngest hottest WD KPD 0005 5106 is very close to 100 000 K of type DO and is the first single WD recorded as an X ray source with ROSAT 11 12 Cataclysmic variables editMain article Cataclysmic variable star Cataclysmic variables CVs are close binary systems consisting of a white dwarf and a red dwarf secondary transferring matter via the Roche lobe overflow 13 Both fusion and accretion powered cataclysmic variables have been observed to be X ray sources 14 The accretion disk may be prone to instability leading to dwarf nova outbursts a portion of the disk material falls onto the white dwarf the cataclysmic outbursts occur when the density and temperature at the bottom of the accumulated hydrogen layer rise high enough to ignite nuclear fusion reactions which rapidly burn the hydrogen layer to helium Apparently the only SSXS nonmagnetic cataclysmic variable is V Sagittae bolometric luminosity of 1 10 x 1037 a binary including a blackbody BB accretor at T lt 80 eV and an orbital period of 0 514195 d 5 The accretion disk can become thermally stable in systems with high mass transfer rates Ṁ 13 Such systems are called nova like NL stars because they lack outbursts characteristic of dwarf novae 15 VY Scl cataclysmic variables editAmong the NL stars is a small group which shows a temporary reduction or cessation of Ṁ from the secondary These are the VY Scl type stars or anti dwarf novae 16 V751 Cyg edit V751 Cyg BB MW is a VY Scl CV has a bolometric luminosity of 6 5 x 1036 erg s 5 and emits soft X rays at quiescence 17 The discovery of a weak soft X ray source of V751 Cyg at minimum presents a challenge as this is unusual for CVs which commonly display weak hard X ray emission at quiescence 17 The high luminosity 6 5 x 1036 erg s is particularly hard to understand in the context of VY Scl stars generally because observations suggest that the binaries become simple red dwarf white dwarf pairs at quiescence the disk mostly disappears 17 A high luminosity in soft X rays poses an additional problem of understanding why the spectrum is of only modest excitation 17 The ratio He II l4686 Hb did not exceed 0 5 in any of the spectra recorded up to 2001 which is typical for accretion powered CVs and does not approach the ratio of 2 commonly seen in supersoft binaries CBSS 17 Pushing the edge of acceptable X ray fits toward lower luminosity suggests that the luminosity should not exceed 2 x 1033 ergs s which gives only 4 x 1031 ergs s of reprocessed light in the WD about equal to the secondary s expected nuclear luminosity 17 Magnetic cataclysmic variables editMain article Polar cataclysmic variable X rays from magnetic cataclysmic variables are common because accretion provides a continuous supply of coronal gas 18 A plot of number of systems vs orbit period shows a statistically significant minimum for periods between 2 and 3 hr which can probably be understood in terms of the effects of magnetic braking when the companion star becomes completely convective and the usual dynamo which operates at the base of the convective envelope can no longer give the companion a magnetic wind to carry off angular momentum 18 The rotation has been blamed on asymmetric ejection of planetary nebulae and winds 19 and the fields on in situ dynamos 20 Orbit and rotation periods are synchronized in strongly magnetized WDs 18 Those with no detectable field never are synchronized With temperatures in the range 11 000 to 15 000 K all the WDs with the most extreme fields are far too cool to be detectable EUV X ray sources e g Grw 70 8247 LB 11146 SBS 1349 5434 PG 1031 234 and GD 229 21 Most highly magnetic WDs appear to be isolated objects although G 23 46 7 4 MG and LB 1116 670 MG are in unresolved binary systems 22 RE J0317 853 is the hottest magnetic WD at 49 250 K with an exceptionally intense magnetic field of 340 MG and implied rotation period of 725 4 s 22 Between 0 1 and 0 4 keV RE J0317 853 was detectable by ROSAT but not in the higher energy band from 0 4 to 2 4 keV citation needed RE J0317 853 is associated with a blue star 16 arcsec from LB 9802 also a blue WD but not physically associated 22 A centered dipole field is not able to reproduce the observations but an off center dipole 664 MG at the south pole and 197 MG at the north pole does 22 Until recently 1995 only PG 1658 441 possessed an effective temperature gt 30 000 K 22 Its polar field strength is only 3 MG 22 The ROSAT Wide Field Camera WFC source RE J0616 649 has an 20 MG field 23 PG 1031 234 has a surface field that spans the range from 200 MG to nearly 1000 MG and rotates with a period of 3h24m 24 The magnetic fields in CVs are confined to a narrow range of strengths with a maximum of 7080 MG for RX J1938 4 4623 25 None of the single magnetic stars has been seen as of 1999 as an X ray source although fields are of direct relevance to the maintenance of coronae in main sequence stars 18 PG 1159 stars editPG 1159 stars are a group of very hot often pulsating WDs for which the prototype is PG 1159 dominated by carbon and oxygen in their atmospheres 18 PG 1159 stars reach luminosities of 1038 erg s but form a rather distinct class 26 RX J0122 9 7521 has been identified as a galactic PG 1159 star 27 28 Nova editMain article Nova There are three SSXSs with bolometric luminosity of 1038 erg s that are novae GQ Mus BB MW V1974 Cyg WD MW and Nova LMC 1995 WD 5 Apparently as of 1999 the orbital period of Nova LMC 1995 if a binary was not known U Sco a recurrent nova as of 1999 unobserved by ROSAT is a WD 74 76 eV Lbol 8 60 x 1036 erg s with an orbital period of 1 2306 d 5 Planetary nebula editMain article Planetary nebula In the SMC 1E 0056 8 7154 is a WD with bolometric luminosity of 2 x 1037 that has a planetary nebula associated with it 5 Super soft active galactic nuclei editSupersoft active galactic nuclei reach luminosities up to 1045 erg s 5 Large amplitude outbursts editLarge amplitude outbursts of super soft X ray emission have been interpreted as tidal disruption events 29 See also editCarbon detonation Type Ia supernova X ray astronomyReferences edit Supersoft X Ray Sources Archived from the original on 2008 06 07 a b c d White NE Giommi P Heise J Angelini L et al 1995 RX J0045 4 4154 A Recurrent Supersoft X ray Transient in M31 The Astrophysical Journal 445 L125 Bibcode 1995ApJ 445L 125W doi 10 1086 187905 Archived from the original on 2009 07 03 a b c d e Kahabka P Dec 2006 Supersoft X ray sources Advances in Space Research 38 12 2836 9 Bibcode 2006AdSpR 38 2836K doi 10 1016 j asr 2005 10 058 Max Planck Institute for Extraterrestrial Physics Super Soft X ray Sources Discovered with ROSAT a b c d e f g h i j k l Greiner J 2000 Catalog of supersoft X ray sources New Astronomy 5 3 137 41 arXiv astro ph 0005238 Bibcode 2000NewA 5 137G doi 10 1016 S1384 1076 00 00018 X S2CID 52241439 Max Planck Institute for Extraterrestrial Physics Proceedings of the Workshop on Supersoft X ray Sources Catalog of Supersoft X ray Sources Archived from the original on 2007 11 28 a b Kahabka P van den Heuvel EPJ 1997 Luminous Supersoft X Ray Sources PDF Annual Review of Astronomy and Astrophysics 35 1 69 100 Bibcode 1997ARA amp A 35 69K doi 10 1146 annurev astro 35 1 69 S2CID 70774203 a b Schmidtke PC Cowley AP Sep 2001 Synoptic Observations of the Supersoft Binary MR Velorum RX J0925 7 4758 Determination of the Orbital Period The Astronomical Journal 122 3 1569 71 Bibcode 2001AJ 122 1569S doi 10 1086 322155 David Darling site symbiotic star description Fleming TA Werner K Barstow MA October 1993 Detection of the First Coronal X Ray Source about a White Dwarf The Astrophysical Journal 416 L79 Bibcode 1993ApJ 416L 79F doi 10 1086 187075 Werner 1994 Spectral analysis of the hottest known helium rich white dwarf KPD 0005 5106 Astronomy and Astrophysics 284 907 Bibcode 1994A amp A 284 907W a b Kato T Ishioka R Uemura M Dec 2002 Photometric Study of KR Aurigae during the High State in 2001 Publications of the Astronomical Society of Japan 54 6 1033 9 arXiv astro ph 0209351 Bibcode 2002PASJ 54 1033K doi 10 1093 pasj 54 6 1033 Introduction to Cataclysmic Variables CVs Osaki Yoji 1996 Dwarf 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Astrophysical Journal 448 305 Bibcode 1995ApJ 448 305S doi 10 1086 175962 a b c d e f Barstow MA Jordan S O Donoghue D Burleigh MR et al 1995 RE J0317 853 the hottest known highly magnetic DA white dwarf Monthly Notices of the Royal Astronomical Society 277 3 931 85 Bibcode 1995MNRAS 277 971B doi 10 1093 mnras 277 3 971 Barstow M A Jordan S O Donoghue D Burleigh M R et al December 1995 RE J0317 853 the hottest known highly magnetic DA white dwarf Monthly Notices of the Royal Astronomical Society 277 3 971 985 Bibcode 1995MNRAS 277 971B doi 10 1093 mnras 277 3 971 Latter WB Schmidt GD Green RF 1987 The rotationally modulated Zeeman spectrum at nearly 10 to the 9th Gauss of the white dwarf PG 1031 234 The Astrophysical Journal 320 308 Bibcode 1987ApJ 320 308L doi 10 1086 165543 Schwope AD et al 1995 Two pole accretion in the high field polar RXJ 1938 6 4612 Astronomy and Astrophysics 293 764 Bibcode 1995A amp A 293 764S Dreizler S Werner K Heber U 1995 PG 1159 stars and their 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