4U 1700-37

{{Starbox begin}}

{{Starbox image

| image = 250px

| caption = A light curve for V884 Scorpii. The main plot, from TESS data, shows the variation over several orbital periods. The inset plot, adapted from van Paradijs et al. (1984), shows the average variation as a function of orbit phase.

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{{Starbox observe

|epoch=J2000

|constell=Scorpius

|ra={{RA|17|03|56.77256}}

|dec={{DEC|-37|50|38.9133}}

|appmag_v=6.51 (- 6.57) - 6.60

}}

{{Starbox character

|class=O6Iafcp{{cite journal|bibcode=2014ApJS..211...10S|doi=10.1088/0067-0049/211/1/10|arxiv=1312.6222|title=The Galactic O-Star Spectroscopic Survey (GOSSS). II. Bright Southern Stars|journal=The Astrophysical Journal Supplement Series|volume=211|issue=1|pages=10|year=2014|last1=Sota|first1=A.|last2=Apellániz|first2=J. Maíz|last3=Morrell|first3=N. I.|last4=Barbá|first4=R. H.|last5=Walborn|first5=N. R.|last6=Gamen|first6=R. C.|last7=Arias|first7=J. I.|last8=Alfaro|first8=E. J.|s2cid=118847528}}

|b-v=+0.253{{cite journal|bibcode=1985A&AS...61..387K|title=Photometric observations of emission B-stars in the southern Milky Way|author=Kozok, J. R.|journal=Astronomy and Astrophysics Supplement Series|volume=61|pages=387–405|date=1985}}

|u-b=−0.727{{cite journal|bibcode=1985A&AS...61..387K|title=Photometric observations of emission B-stars in the southern Milky Way|author=Kozok, J. R.|journal=Astronomy and Astrophysics Supplement Series|volume=61|pages=387–405|date=1985}}

|variable=Ellipsoidal + HMXB{{cite journal|bibcode=2009yCat....102025S|title=VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)|journal=VizieR On-line Data Catalog: B/gcvs. Originally Published in: 2009yCat....102025S|volume=1|display-authors=etal|last1=Samus|first1=N. N.|last2=Durlevich|first2=O. V.|year=2009}}

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{{Starbox astrometry

|radial_v= {{val|−75.00|7.4}}{{cite journal|title=Astrophysical supplements to the ASCC-2.5: Ia. Radial velocities of ~55000 stars and mean radial velocities of 516 Galactic open clusters and associations|author=Kharchenko, N. V.|display-authors=etal|journal=Astronomische Nachrichten|volume=328|issue=9|page=889|date=2007|bibcode=2007AN....328..889K|doi=10.1002/asna.200710776|arxiv=0705.0878|s2cid=119323941}}

|prop_mo_ra=2.414

|prop_mo_dec=5.022

|parallax=0.6327

|p_error=0.0259

|parallax_footnote={{cite Gaia EDR3|5976382915813535232}}

|dist_ly=

|dist_pc=

|absmag_v=−6.52{{citation |postscript=. |bibcode=2020Ap&SS.365..112M |title=Distance scale for high-luminosity stars in OB associations and in field with Gaia DR2. Spurious systematic motions |last1=Melnik |first1=A. M. |last2=Dambis |first2=A. K. |journal=Astrophysics and Space Science |year=2020 |volume=365 |issue=7 |page=112 |doi=10.1007/s10509-020-03827-0 |arxiv=2006.14649 |s2cid=220128144 }}

}}

{{Starbox orbit

|reference={{cite journal|title=S_B⁹: The ninth catalogue of spectroscopic binary orbits|display-authors=1|author1=Pourbaix, D.|author2=Tokovinin, A. A.|author3=Batten, A. H.|author4=Fekel, F. C.|author5=Hartkopf, W. I.|author6=Levato, H.|author7=Morrell, N. I.|author8=Torres, G.|author9=Udry, S.|journal=Astronomy and Astrophysics|volume=424|issue=2|pages=727–732|year=2004|doi=10.1051/0004-6361:20041213|arxiv=astro-ph/0406573|bibcode=2004A&A...424..727P|s2cid=119387088}}

|period_unitless=3.4118 ± 0.0001 d

|axis=

|inclination=

|node=

|periastron={{nowrap|JD {{val|2443702.62|0.21}}}}

|eccentricity={{val|0.17|0.06}}

|periarg_primary={{val|54|24}}

|k1=10.06 ± 0.66

}}

{{Starbox detail

|source={{cite journal|bibcode=2002A&A...392..909C|doi=10.1051/0004-6361:20021184|arxiv=astro-ph/0207334|title=Physical parameters of the high-mass X-ray binary 4U1700-37|journal=Astronomy & Astrophysics|volume=392|issue=3|pages=909–920|year=2002|last1=Clark|first1=J. S.|last2=Goodwin|first2=S. P.|last3=Crowther|first3=P. A.|last4=Kaper|first4=L.|last5=Fairbairn|first5=M.|last6=Langer|first6=N.|last7=Brocksopp|first7=C.|s2cid=119552560}}

|component1=O star

|mass={{val|58|11}}

|radius={{val|21.9|+1.3|-0.5}}

|temperature={{val|35000|1000|fmt=commas}}

|luminosity=660,000

|component2=X-ray object

|mass2={{val|2.44|0.27}}

}}

{{Starbox catalog

|names={{odlist|V=V884 Sco|CD=-37°11206|HD=153919|HIP=83499|SAO=208356}}{{cite simbad|title=HD 153919|access-date=4 September 2017}}

}}

{{Starbox reference

|Simbad=HD+153919

}}

{{Starbox end}}

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.{{cite journal|bibcode=1973ApJ...181L..43J|doi=10.1086/181181|title=Evidence for the Binary Nature of 2U 1700-37|journal=The Astrophysical Journal|volume=181|pages=L43|year=1973|last1=Jones|first1=C.|last2=Forman|first2=W.|last3=Tananbaum|first3=H.|last4=Schreier|first4=E.|last5=Gursky|first5=H.|last6=Kellogg|first6=E.|last7=Giacconi|first7=R.|doi-access=free}} 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;{{cite journal|arxiv=1710.01907|title=Evidence of Compton cooling during an X-ray flare supports a neutron star nature of the compact object in 4U1700−37|journal= Monthly Notices of the Royal Astronomical Society: Letters|volume=473|issue=1|pages=L74–L78|year=2018|last1=Martinez-Chicharro|first1=M.|last2=Torrej ́on|first2=J. M.|last3=Oskinova|first3=L.|last4=F ̈urst|first4=F.|last5=Postnov|first5=K.|last6=Rodes-Roca|first6=J. J.|last7=Hainich|first7=R.|last8=Bodaghee|first8=A.|doi=10.1093/mnrasl/slx165|doi-access=free |bibcode=2018MNRAS.473L..74M|s2cid=56539478}} 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 {{val|63|5|u=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.{{cite journal|doi=10.1051/0004-6361/202040114|title=Confirming NGC 6231 as the parent cluster of the runaway high-mass X-ray binary HD 153919/4U 1700-37 with Gaia DR2|year=2021|last1=Van Der Meij|first1=Vincent|last2=Guo|first2=Difeng|last3=Kaper|first3=Lex|last4=Renzo|first4=Mathieu|journal=Astronomy & Astrophysics|volume=655|pages=A31|arxiv=2108.12918|bibcode=2021A&A...655A..31V|s2cid=237353522}}