4U 1700-37

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4U 1700-37
V884ScoLightCurve.png
A light curve for V884 Scorpii. The main plot, from TESS data, [1] shows the variation over several orbital periods. The inset plot, adapted from van Paradijs et al. (1984), [2] shows the average variation as a function of orbit phase.
Observation data
Epoch J2000        Equinox J2000
Constellation Scorpius
Right ascension 17h 03m 56.77256s [3]
Declination −37° 50′ 38.9133″ [3]
Apparent magnitude  (V)6.51 (- 6.57) - 6.60 [4]
Characteristics
Spectral type O6Iafcp [5]
U−B color index −0.727 [6]
B−V color index +0.253 [6]
Variable type Ellipsoidal + HMXB [4]
Astrometry
Radial velocity (Rv)−75.00±7.4 [7]  km/s
Proper motion (μ)RA: 2.414 [3]   mas/yr
Dec.: 5.022 [3]   mas/yr
Parallax (π)0.6327 ± 0.0259  mas [3]
Distance 5,200 ± 200  ly
(1,580 ± 60  pc)
Absolute magnitude  (MV)−6.52 [8]
Orbit [9]
Period (P)3.4118 ± 0.0001 d
Eccentricity (e)0.17±0.06
Periastron epoch (T)JD 2443702.62±0.21
Argument of periastron (ω)
(primary)		54±24°
Semi-amplitude (K1)
(primary)		10.06 ± 0.66 km/s
Details [10]
O star
Mass 58±11  M☉
Radius 21.9+1.3
−0.5  R☉
Luminosity 660,000  L☉
Temperature 35,000±1,000  K
X-ray object
Mass 2.44±0.27  M☉
Other designations
V884 Sco, CD−37°11206, HD  153919, HIP  83499, SAO  208356 [11]
Database references
SIMBAD data

4U 1700-37 is one of the stronger binary X-ray sources in the sky, and is classified as a high-mass X-ray binary. It was discovered by the Uhuru satellite. [12] The "4U" designation refers to the fourth (and final) Uhuru catalog.

The X-ray source is associated with a bright (6.53 V magnitude) blue supergiant star HD 153919, which is orbited by an accreting compact object that must be either a neutron star or a black hole. The X-ray source is eclipsed by the star every 3.4 days, but no pulsations have yet been observed. The source is one of the ten brightest persistent X-ray sources in the 10-100 keV hard X-ray energy region.

Evidence of Compton cooling during an X-ray flare recorded by the Chandra X-ray telescope strongly suggests that the compact object is a neutron star; [13] if verified it would be among the most massive known, and near the boundary of the theoretical maximum.

4U 1700-37 is a runaway system. It has a high velocity of 63±5 km/s with respect to its parent cluster, NGC 6231. It was kicked out of the cluster about 2.2 million years ago by a supernova explosion. [14]

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References

  1. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  2. ↑ van Paradijs, J.; van Amerongen, S.; van der Woerd, H.; Tjemkes, S.; Menzies, J. W. (January 1984). "Optical photometry of massive X-ray binaries: 4U1700-37/HD 153919 = V884 Sco". Astronomy and Astrophysics Supplement Series. 55: 7–14. Bibcode:1984A&AS...55....7V.
  3. 1 2 3 4 5 Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics . 649: A1. arXiv: 2012.01533 . Bibcode:2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657 . S2CID   227254300. (Erratum:  doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  4. 1 2 Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/gcvs. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  5. ↑ Sota, A.; Apellániz, J. Maíz; Morrell, N. I.; Barbá, R. H.; Walborn, N. R.; Gamen, R. C.; Arias, J. I.; Alfaro, E. J. (2014). "The Galactic O-Star Spectroscopic Survey (GOSSS). II. Bright Southern Stars". The Astrophysical Journal Supplement Series. 211 (1): 10. arXiv: 1312.6222 . Bibcode:2014ApJS..211...10S. doi:10.1088/0067-0049/211/1/10. S2CID   118847528.
  6. 1 2 Kozok, J. R. (1985). "Photometric observations of emission B-stars in the southern Milky Way". Astronomy and Astrophysics Supplement Series. 61: 387–405. Bibcode:1985A&AS...61..387K.
  7. ↑ Kharchenko, N. V.; et al. (2007). "Astrophysical supplements to the ASCC-2.5: Ia. Radial velocities of ~55000 stars and mean radial velocities of 516 Galactic open clusters and associations". Astronomische Nachrichten. 328 (9): 889. arXiv: 0705.0878 . Bibcode:2007AN....328..889K. doi:10.1002/asna.200710776. S2CID   119323941.
  8. ↑ Melnik, A. M.; Dambis, A. K. (2020), "Distance scale for high-luminosity stars in OB associations and in field with Gaia DR2. Spurious systematic motions", Astrophysics and Space Science, 365 (7): 112, arXiv: 2006.14649 , Bibcode:2020Ap&SS.365..112M, doi:10.1007/s10509-020-03827-0, S2CID   220128144.
  9. ↑ Pourbaix, D.; et al. (2004). "SB9: The ninth catalogue of spectroscopic binary orbits". Astronomy and Astrophysics. 424 (2): 727–732. arXiv: astro-ph/0406573 . Bibcode:2004A&A...424..727P. doi:10.1051/0004-6361:20041213. S2CID   119387088.
  10. ↑ Clark, J. S.; Goodwin, S. P.; Crowther, P. A.; Kaper, L.; Fairbairn, M.; Langer, N.; Brocksopp, C. (2002). "Physical parameters of the high-mass X-ray binary 4U1700-37". Astronomy & Astrophysics. 392 (3): 909–920. arXiv: astro-ph/0207334 . Bibcode:2002A&A...392..909C. doi:10.1051/0004-6361:20021184. S2CID   119552560.
  11. ↑ "HD 153919". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 4 September 2017.
  12. ↑ Jones, C.; Forman, W.; Tananbaum, H.; Schreier, E.; Gursky, H.; Kellogg, E.; Giacconi, R. (1973). "Evidence for the Binary Nature of 2U 1700-37". The Astrophysical Journal. 181: L43. Bibcode:1973ApJ...181L..43J. doi: 10.1086/181181 .
  13. ↑ Martinez-Chicharro, M.; Torrej ́on, J. M.; Oskinova, L.; F ̈urst, F.; Postnov, K.; Rodes-Roca, J. J.; Hainich, R.; Bodaghee, A. (2018). "Evidence of Compton cooling during an X-ray flare supports a neutron star nature of the compact object in 4U1700−37". Monthly Notices of the Royal Astronomical Society: Letters. 473 (1): L74–L78. arXiv: 1710.01907 . Bibcode:2018MNRAS.473L..74M. doi: 10.1093/mnrasl/slx165 . S2CID   56539478.
  14. ↑ Van Der Meij, Vincent; Guo, Difeng; Kaper, Lex; Renzo, Mathieu (2021). "Confirming NGC 6231 as the parent cluster of the runaway high-mass X-ray binary HD 153919/4U 1700-37 with Gaia DR2". Astronomy & Astrophysics. 655: A31. arXiv: 2108.12918 . Bibcode:2021A&A...655A..31V. doi:10.1051/0004-6361/202040114. S2CID   237353522.
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