Astronomy: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
Equinox J2000.0]] (ICRS)
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[3] mas
Distance5,200 ± 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 periapsis (ω)
(primary)		54±24°
Semi-amplitude (K1)
(primary)		10.06 ± 0.66 km/s
Details[10]
O star
Mass58±11 M☉
Radius21.9+1.3
−0.5 R☉
Luminosity660,000 L☉
Temperature35,000±1,000 K
X-ray object
Mass2.44±0.27 M☉
Other designations
V884 Sco, CD−37°11206, HD 153919, HIP 83499, SAO 208356[11]
Database references
SIMBADdata

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]

References

  1. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html. 
  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. ↑ 3.0 3.1 3.2 3.3 3.4 Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G.  Gaia EDR3 record for this source at VizieR.
  4. ↑ 4.0 4.1 Samus, N. N. 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. doi:10.1088/0067-0049/211/1/10. Bibcode: 2014ApJS..211...10S. 
  6. ↑ 6.0 6.1 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. (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. doi:10.1002/asna.200710776. Bibcode: 2007AN....328..889K. 
  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, doi:10.1007/s10509-020-03827-0, Bibcode: 2020Ap&SS.365..112M. 
  9. ↑ Pourbaix, D. et al. (2004). "SB9: The ninth catalogue of spectroscopic binary orbits". Astronomy and Astrophysics 424 (2): 727–732. doi:10.1051/0004-6361:20041213. Bibcode: 2004A&A...424..727P. 
  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. doi:10.1051/0004-6361:20021184. Bibcode: 2002A&A...392..909C. 
  11. ↑ "HD 153919". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+153919. 
  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. doi:10.1086/181181. Bibcode: 1973ApJ...181L..43J. 
  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. doi:10.1093/mnrasl/slx165. Bibcode: 2018MNRAS.473L..74M. 
  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. doi:10.1051/0004-6361/202040114. Bibcode: 2021A&A...655A..31V. 

External links

  • Seifina, Elena; Titarchuk, Lev; Shaposhnikov, Nikolai (2016). "X-Ray Spectra of the High-Mass X-Ray Binary 4U 1700-37 Usingbepposax, Suzaku, Andrxteobservations". The Astrophysical Journal 821 (1): 23. doi:10.3847/0004-637X/821/1/23. Bibcode: 2016ApJ...821...23S. 
  • Jaisawal, G. K.; Naik, S. (2015). "Broad-band spectroscopy of the eclipsing high-mass X-ray binary 4U 1700-37 with Suzaku". Monthly Notices of the Royal Astronomical Society 448 (1): 620–628. doi:10.1093/mnras/stv029. Bibcode: 2015MNRAS.448..620J. 
  • Giménez-García, A.; Torrejón, J. M.; Eikmann, W.; Martínez-Núñez, S.; Oskinova, L. M.; Rodes-Roca, J. J.; Bernabéu, G. (2015). "An XMM-Newton view of FeKα in high-mass X-ray binaries". Astronomy & Astrophysics 576: A108. doi:10.1051/0004-6361/201425004. Bibcode: 2015A&A...576A.108G. 
  • Islam, Nazma; Paul, Biswajit (2016). "Orbital evolution and search for eccentricity and apsidal motion in the eclipsing HMXB 4U 1700−37". Monthly Notices of the Royal Astronomical Society 461 (1): 816–824. doi:10.1093/mnras/stw1299. Bibcode: 2016MNRAS.461..816I. 



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