Super soft X-ray source

From Wikipedia, the free encyclopedia
Jump to: navigation, search

A super soft X-ray source (SSXS, or SSS) is an astronomical source of very low energy 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] SSXSs are in most cases only detected below 0.5 keV, so that within our own galaxy they are usually 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 SSSs 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 (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]

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 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]

"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 Sge: 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]

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.[20]

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.[21]

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.[21] 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.[22] RE J0317-853 is associated with a blue star 16 arcsec from LB 9802 (also a blue WD) but not physically associated.[21] 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.[21]

Until recently (1995) only PG 1658+441 possessed an effective temperature > 30,000 K.[21] Its polar field strength is only 3 MG.[21]

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]

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]

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. ^ "Supersoft X-Ray Sources". 
  2. ^ a b c d White NE, Giommi P, Heise J, Angelini L, Fantasia S. "RX J0045.4+4154: A Recurrent Supersoft X-ray Transient in M31". Ap J Lett. 445: L125. 
  3. ^ a b c d e Kahabka P (Dec 2006). "Supersoft X-ray sources". Adv Space Res. 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 Astron. 5 (3): 137–41. arXiv:astro-ph/0005238. Bibcode:2000NewA....5..137G. doi:10.1016/S1384-1076(00)00018-X. 
  6. ^ Max Planck Institute for Extraterrestrial Physics. "Proceedings of the Workshop on Supersoft X-ray Sources". 
  7. ^ "Catalog of Supersoft X-ray Sources". 
  8. ^ a b Kahabka P, van den Heuvel EPJ (1997). "Luminous Supersoft X-Ray Sources". Ann Rev Astron Astrophys. 35 (1): 69–100. Bibcode:1997ARA&A..35...69K. doi:10.1146/annurev.astro.35.1.69. 
  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". Astron J. 122 (3): 1569–71. Bibcode:2001AJ....122.1569S. doi:10.1086/322155. 
  10. ^ "David Darling site symbiotic star description". 
  11. ^ Fleming TA "et al." (1994). Ap J. 411: L79. 
  12. ^ Werner (1994). Astron Astrophys. 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". Publ Astron Soc Japan 54 (6): 1033–9. arXiv:astro-ph/0209351. Bibcode:2002PASJ...54.1033K. 
  14. ^ "Introduction to Cataclysmic Variables (CVs)". 
  15. ^ Osaki, Yoji (1996). "Dwarf-Nova Outbursts". PASP 108: 39. Bibcode:1996PASP..108...39O. doi:10.1086/133689. 
  16. ^ Warner B (1995). Cataclysmic Variable Stars. Cambridge: Cambridge University Press. 
  17. ^ a b c d e f Patterson J, Thorstensen JR, Fried R, Skillman DR, Cook LM, Jensen L (Jan 2001). "Superhumps in Cataclysmic Binaries. XX. V751 Cygni". Publ Astron Soc Pacific (PASP) 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 1990's". Bull Astron Soc India. 27: 549–66. Bibcode:1999BASI...27..549T. 
  19. ^ Spruit HC (1998). Astron Astrophys. 333: 603. arXiv:astro-ph/9802141. Bibcode:1998A&A...333..603S. 
  20. ^ a b Schmidt GD, Grauer AD (1997). "Upper Limits for Magnetic Fields on Pulsating White Dwarfs". Ap J. 488 (2): 827. Bibcode:1997ApJ...488..827S. doi:10.1086/304746. 
  21. ^ a b c d e f Barstow MA, Jordan S, O'Donoghue D, Burleigh MR, Napiwotzki R, Harrop-Allin MK (1995). "RE J0317-853: the hottest known highly magnetic DA white dwarf". MNRAS 277 (3): 931–85. Bibcode:1995MNRAS.277..971B. 
  22. ^ Fleming TA (1995). Astron Astrophys. 
  23. ^ Jordan, Finley.  Missing or empty |title= (help)
  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". Ap J. 320: 308. Bibcode:1987ApJ...320..308L. doi:10.1086/165543. 
  25. ^ Schwope AD, "et al." (1995). Astron Astrophys. 293: 764. Bibcode:1995A&A...293..764S. 
  26. ^ Dreizler S, Werner K, Heber U (1995). "White Dwarfs". In Kӧster D, Werner K. Lect Notes Phys. (Berlin: Springer) 443: 160. 
  27. ^ Cowley AP, Schmidtke PC, Hutchings JB, Crampton D (1995). "X-Ray Discovery of a Hot PG1159 Star, RX J0122.9-7521". PASP 107: 927. Bibcode:1995PASP..107..927C. doi:10.1086/133640. 
  28. ^ Werner K, Wolff B, Cowley AP, Schmidtke PC, Hutchings JB, Crampton D, (1996). "Supersoft X-ray Sources". In Greiner. Lect Notes Phys. (Berlin: Springer) 472: 131. 
  29. ^ Komossa S, Greiner J (1999). Astron Astrophys. 349: L45. arXiv:astro-ph/9908216. Bibcode:1999A&A...349L..45K.