# V752 Centauri

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Star in the constellation Centaurus

V752 Centauri A visual band light curve for V752 Centauri, plotted from data presented by Sisteró and Castore de Sisteró (1973)[1] Observation data Epoch J2000 Equinox J2000 Constellation Centaurus Right ascension 11h 42m 48.08s[2] Declination −35° 48′ 57.5″[2] Apparent magnitude (V) 9.10 – 9.66[3] Characteristics Evolutionary stage F7/G0(V)[4] Variable type W UMa[5] Astrometry Proper motion (μ) RA: −52.175[2] mas/yr Dec.: −24.364[2] mas/yr Parallax (π) 7.9641±0.0495 mas[2] Distance 410 ± 3 ly (125.6 ± 0.8 pc) Absolute magnitude (MV) 4.00 ± 0.34[6] Orbit Period (P) 0.37023198 days[7] Semi-major axis (a) 2.59 ± 0.05 R☉[7] Inclination (i) 82.07 ± 0.06[7]° Semi-amplitude (K1) (primary) 83.2±5.7[8] km/s Semi-amplitude (K2) (secondary) 267.2±6.9[8] km/s Details Age 3.84[9] Gyr Primary Mass 1.31 ± 0.07[7] M☉ Radius 1.30 ± 0.02[7] R☉ Luminosity 2.00 ± 0.07}[7] L☉ Temperature 5,955 ± 77[5] K Secondary Mass 0.39 ± 0.02[7] M☉ Radius 0.77 ± 0.01[7] R☉ Luminosity 0.75 ± 0.03[7] L☉ Temperature 6,221 ± 81[5] K Other designations V752 Cen, CD−35°7392, HD 101799, HIP 57129, SAO 202729[10] Database references SIMBAD data

**V752 Centauri** (HD 101799) is [multiple star system](/source/Multiple_star_system)[11] and [variable star](/source/Variable_star) in the [constellation](/source/Constellation) of [Centaurus](/source/Centaurus_(constellation)). An [eclipsing binary](/source/Eclipsing_binary), its [apparent magnitude](/source/Apparent_magnitude) has a maximum of 9.10, dimming to 9.66 during primary eclipse and 9.61 during secondary eclipse.[3] Its variability was discovered by Howard Bond in 1970.[12] From [parallax](/source/Parallax) measurements by the [Gaia](/source/Gaia_(spacecraft)) spacecraft, the system is located at a distance of 410 [light-years](/source/Light-year) (125.6 [parsecs](/source/Parsec)) from Earth.[2]

V752 Centauri is a [contact binary](/source/Contact_binary) of the [W Ursae Majoris](/source/W_Ursae_Majoris_variable) type, composed of two F-type stars with a combined [spectral type](/source/Spectral_type) of F7/G0(V).[4] Individually, the components have been classified as F8 + F5,[8] and F8 + F7.5.[13] With [effective temperatures](/source/Effective_temperature) of 5,955 and 6,221 [K](/source/Kelvin),[5] the system is classified as a W Ursae Majoris variable of subtype W, where the secondary star is hotter than the primary; for this reason, the primary eclipses are caused by the occultation of the secondary star.[8][5] The system has an [orbital period](/source/Orbital_period) of only 0.3702 days and a separation of 2.59 [solar radii](/source/Solar_radius). The orbit is [inclined](/source/Inclination) by 82° in relation to the plane of the sky.[7]

The combination of [photometric](/source/Photometry_(astronomy)) and spectroscopic data have allowed the direct determination of the parameters of the stars. The primary component has a mass of 1.31 times the [solar mass](/source/Solar_mass), radius of 1.30 times the solar radius and a [luminosity](/source/Luminosity) double that of [the Sun](/source/Solar_luminosity). The secondary has only 0.39 times the solar mass, 0.77 times the solar radius, and 0.75 times the solar luminosity.[7] Since the stars are in contact, there is considerable [mass transfer](/source/Mass_transfer) from the secondary to the primary. It is estimated that the secondary star was initially the more massive star, with 1.76 times the solar mass, while the primary had an initial mass of 0.84 time the solar mass.[9] The system's age is estimated at 3.8 billion years.[9] All contact binary stars are expected to eventually merge into a single, fast-rotating star.[14]

The system's spectrum shows the [spectral lines](/source/Spectral_line) of a third star, which seems to be a [K-type main sequence star](/source/K-type_main_sequence_star). This third star is itself a [spectroscopic binary](/source/Spectroscopic_binary) with a period of 5.147 days, with a small companion that is probably an M-type [red dwarf](/source/Red_dwarf). The V752 Centauri system is thus composed of four stars, with two binary pairs that orbit each other.[11] Most contact binary stars have one or more distant companions, and were possibly formed by [angular momentum](/source/Angular_momentum) loss due to gravitational interactions with these companion stars.[15][7]

The [light curve](/source/Light_curve) analysis of V752 Centauri reveals that between 1970 and 2000, the orbital period of the eclipsing binary remained approximately constant, indicating there was no significant mass transfer. Around the year 2000, the period abruptly increased, possibly accompanied by a slightly dimmer primary eclipse.[16] Since then, the period has been increasing at a rate of 0.044 seconds per year, which is caused by mass transfer from the less massive star to the more massive one at a rate of 2.52×10−7 M☉ per year. This period change and the beginning of the mass transfer phase were possibly caused by interactions with the companion binary star.[7]

## References

1. **[^](#cite_ref-Sisteró_1-0)** Sisteró, R. F.; Castore de Sisteró, M. E. (June 1973). ["UBV light variation and orbital elements of HD 101799"](https://doi.org/10.1086%2F111435). *The Astronomical Journal*. **78** (5): 413–421. [Bibcode](/source/Bibcode_(identifier)):[1973AJ.....78..413S](https://ui.adsabs.harvard.edu/abs/1973AJ.....78..413S). [doi](/source/Doi_(identifier)):[10.1086/111435](https://doi.org/10.1086%2F111435).

1. ^ [***a***](#cite_ref-GaiaDR2_2-0) [***b***](#cite_ref-GaiaDR2_2-1) [***c***](#cite_ref-GaiaDR2_2-2) [***d***](#cite_ref-GaiaDR2_2-3) [***e***](#cite_ref-GaiaDR2_2-4) [***f***](#cite_ref-GaiaDR2_2-5) [Brown, A. G. A.](/source/Anthony_Brown_(scientist)); et al. ([Gaia collaboration](/source/Data_Processing_and_Analysis_Consortium)) (August 2018). ["*Gaia* Data Release 2: Summary of the contents and survey properties"](https://doi.org/10.1051%2F0004-6361%2F201833051). *[Astronomy & Astrophysics](/source/Astronomy_%26_Astrophysics)*. **616**. A1. [arXiv](/source/ArXiv_(identifier)):[1804.09365](https://arxiv.org/abs/1804.09365). [Bibcode](/source/Bibcode_(identifier)):[2018A&A...616A...1G](https://ui.adsabs.harvard.edu/abs/2018A&A...616A...1G). [doi](/source/Doi_(identifier)):[10.1051/0004-6361/201833051](https://doi.org/10.1051%2F0004-6361%2F201833051). [Gaia DR2 record for this source](https://vizier.u-strasbg.fr/viz-bin/VizieR-S?Gaia%20DR2%203464532418676024064) at [VizieR](/source/VizieR).

1. ^ [***a***](#cite_ref-Avvakumova2013_3-0) [***b***](#cite_ref-Avvakumova2013_3-1) Avvakumova, E. A.; Malkov, O. Yu.; Kniazev, A. Yu. (2013). "Eclipsing variables: Catalogue and classification". *Astronomische Nachrichten*. **334** (8): 860. [Bibcode](/source/Bibcode_(identifier)):[2013AN....334..860A](https://ui.adsabs.harvard.edu/abs/2013AN....334..860A). [doi](/source/Doi_(identifier)):[10.1002/asna.201311942](https://doi.org/10.1002%2Fasna.201311942). [hdl](/source/Hdl_(identifier)):[10995/27061](https://hdl.handle.net/10995%2F27061).

1. ^ [***a***](#cite_ref-HOUK1982_4-0) [***b***](#cite_ref-HOUK1982_4-1) Houk, Nancy (1982), "Michigan Catalogue of Two-dimensional Spectral Types for the HD Stars", *Michigan Catalogue of Two-dimensional Spectral Types for the HD Stars. Volume_3. Declinations -40_ƒ0 to -26_ƒ0*, **3**, Ann Arbor, Michigan: Dept. of Astronomy, University of Michigan, [Bibcode](/source/Bibcode_(identifier)):[1982mcts.book.....H](https://ui.adsabs.harvard.edu/abs/1982mcts.book.....H)

1. ^ [***a***](#cite_ref-Barone1993_5-0) [***b***](#cite_ref-Barone1993_5-1) [***c***](#cite_ref-Barone1993_5-2) [***d***](#cite_ref-Barone1993_5-3) [***e***](#cite_ref-Barone1993_5-4) Barone, F.; Di Fiore, L.; Milano, L.; Russo, G. (1993). "Analysis of Contact Binary Systems: AA Ursae Majoris, V752 Centauri, AO Camelopardalis, and V677 Centauri". *The Astrophysical Journal*. **407**: 237. [Bibcode](/source/Bibcode_(identifier)):[1993ApJ...407..237B](https://ui.adsabs.harvard.edu/abs/1993ApJ...407..237B). [doi](/source/Doi_(identifier)):[10.1086/172509](https://doi.org/10.1086%2F172509).

1. **[^](#cite_ref-Rucinski1997_6-0)** Rucinski, S. M.; Duerbeck, H. W. (1997). ["Absolute Magnitude Calibration for the W UMa-Type Systems Based on HIPPARCOS Data"](https://doi.org/10.1086%2F134014). *Publications of the Astronomical Society of the Pacific*. **109**: 1340. [arXiv](/source/ArXiv_(identifier)):[astro-ph/9710214](https://arxiv.org/abs/astro-ph/9710214). [Bibcode](/source/Bibcode_(identifier)):[1997PASP..109.1340R](https://ui.adsabs.harvard.edu/abs/1997PASP..109.1340R). [doi](/source/Doi_(identifier)):[10.1086/134014](https://doi.org/10.1086%2F134014).

1. ^ [***a***](#cite_ref-Zhou2019_7-0) [***b***](#cite_ref-Zhou2019_7-1) [***c***](#cite_ref-Zhou2019_7-2) [***d***](#cite_ref-Zhou2019_7-3) [***e***](#cite_ref-Zhou2019_7-4) [***f***](#cite_ref-Zhou2019_7-5) [***g***](#cite_ref-Zhou2019_7-6) [***h***](#cite_ref-Zhou2019_7-7) [***i***](#cite_ref-Zhou2019_7-8) [***j***](#cite_ref-Zhou2019_7-9) [***k***](#cite_ref-Zhou2019_7-10) [***l***](#cite_ref-Zhou2019_7-11) [***m***](#cite_ref-Zhou2019_7-12) Zhou, X.; Soonthornthum, B.; Qian, S. -B.; Fernández Lajús, E. (2019). ["V752 Cen – a triple-lined spectroscopic contact binary with sudden and continuous period changes"](https://doi.org/10.1093%2Fmnras%2Fstz2508). *Monthly Notices of the Royal Astronomical Society*. **489** (4): 4760. [arXiv](/source/ArXiv_(identifier)):[1909.06038](https://arxiv.org/abs/1909.06038). [Bibcode](/source/Bibcode_(identifier)):[2019MNRAS.489.4760Z](https://ui.adsabs.harvard.edu/abs/2019MNRAS.489.4760Z). [doi](/source/Doi_(identifier)):[10.1093/mnras/stz2508](https://doi.org/10.1093%2Fmnras%2Fstz2508). [S2CID](/source/S2CID_(identifier)) [202572782](https://api.semanticscholar.org/CorpusID:202572782).

1. ^ [***a***](#cite_ref-Sisteró1974_8-0) [***b***](#cite_ref-Sisteró1974_8-1) [***c***](#cite_ref-Sisteró1974_8-2) [***d***](#cite_ref-Sisteró1974_8-3) Sisteró, R. F.; Castore De Sisteró, M. E. (1974). "Radial velocity curves of HD 101799". *The Astronomical Journal*. **79**: 391. [Bibcode](/source/Bibcode_(identifier)):[1974AJ.....79..391S](https://ui.adsabs.harvard.edu/abs/1974AJ.....79..391S). [doi](/source/Doi_(identifier)):[10.1086/111556](https://doi.org/10.1086%2F111556).

1. ^ [***a***](#cite_ref-Yildiz2014_9-0) [***b***](#cite_ref-Yildiz2014_9-1) [***c***](#cite_ref-Yildiz2014_9-2) Yildiz (2014). ["Origin of W UMa-type contact binaries – age and orbital evolution"](https://doi.org/10.1093%2Fmnras%2Fstt1874). *Monthly Notices of the Royal Astronomical Society*. **437** (1): 185–94. [arXiv](/source/ArXiv_(identifier)):[1310.5526](https://arxiv.org/abs/1310.5526). [Bibcode](/source/Bibcode_(identifier)):[2014MNRAS.437..185Y](https://ui.adsabs.harvard.edu/abs/2014MNRAS.437..185Y). [doi](/source/Doi_(identifier)):[10.1093/mnras/stt1874](https://doi.org/10.1093%2Fmnras%2Fstt1874). [S2CID](/source/S2CID_(identifier)) [119121897](https://api.semanticscholar.org/CorpusID:119121897).

1. **[^](#cite_ref-SIMBAD_10-0)** ["V752 Cen"](http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=V752+Cen). *[SIMBAD](/source/SIMBAD)*. [Centre de données astronomiques de Strasbourg](/source/Centre_de_donn%C3%A9es_astronomiques_de_Strasbourg). Retrieved 14 January 2020.

1. ^ [***a***](#cite_ref-Schumacher2009_11-0) [***b***](#cite_ref-Schumacher2009_11-1) Schumacher, H. (2009). "Analysis of the W UMa-type Eclipsing Binary V752 Centauri". *The Eighth Pacific Rim Conference on Stellar Astrophysics: A Tribute to Kam-Ching Leung*. **404**: 199. [Bibcode](/source/Bibcode_(identifier)):[2009ASPC..404..199S](https://ui.adsabs.harvard.edu/abs/2009ASPC..404..199S).

1. **[^](#cite_ref-Bond1970_12-0)** Bond, Howard E. (1970). ["Three Eclipsing Binaries Found Spectroscopically"](https://doi.org/10.1086%2F129004). *Publications of the Astronomical Society of the Pacific*. **82** (489): 1065. [Bibcode](/source/Bibcode_(identifier)):[1970PASP...82.1065B](https://ui.adsabs.harvard.edu/abs/1970PASP...82.1065B). [doi](/source/Doi_(identifier)):[10.1086/129004](https://doi.org/10.1086%2F129004).

1. **[^](#cite_ref-Leung1976_13-0)** Leung, K. -C (1976). ["The contact binary HD 101799"](https://doi.org/10.1086%2F130049). *Publications of the Astronomical Society of the Pacific*. **88**: 936. [Bibcode](/source/Bibcode_(identifier)):[1976PASP...88..936L](https://ui.adsabs.harvard.edu/abs/1976PASP...88..936L). [doi](/source/Doi_(identifier)):[10.1086/130049](https://doi.org/10.1086%2F130049).

1. **[^](#cite_ref-Gazeas2008_14-0)** Gazeas, K.; Stȩpień, K. (2008). ["Angular momentum and mass evolution of contact binaries"](https://doi.org/10.1111%2Fj.1365-2966.2008.13844.x). *Monthly Notices of the Royal Astronomical Society*. **390** (4): 1577. [arXiv](/source/ArXiv_(identifier)):[0803.0212](https://arxiv.org/abs/0803.0212). [Bibcode](/source/Bibcode_(identifier)):[2008MNRAS.390.1577G](https://ui.adsabs.harvard.edu/abs/2008MNRAS.390.1577G). [doi](/source/Doi_(identifier)):[10.1111/j.1365-2966.2008.13844.x](https://doi.org/10.1111%2Fj.1365-2966.2008.13844.x). [S2CID](/source/S2CID_(identifier)) [14661232](https://api.semanticscholar.org/CorpusID:14661232).

1. **[^](#cite_ref-Pribulla2006_15-0)** Pribulla, T.; Rucinski, S. M. (2006). "Contact Binaries with Additional Components. I. The Extant Data". *The Astronomical Journal*. **131** (6): 2986–3007. [arXiv](/source/ArXiv_(identifier)):[astro-ph/0601610](https://arxiv.org/abs/astro-ph/0601610). [Bibcode](/source/Bibcode_(identifier)):[2006AJ....131.2986P](https://ui.adsabs.harvard.edu/abs/2006AJ....131.2986P). [doi](/source/Doi_(identifier)):[10.1086/503871](https://doi.org/10.1086%2F503871). [S2CID](/source/S2CID_(identifier)) [15762240](https://api.semanticscholar.org/CorpusID:15762240).

1. **[^](#cite_ref-Mallama2015_16-0)** Mallama, A.; Pavlov, H. (2015). "Sudden Period Change and Dimming of the Eclipsing Binary V752 Centauri". *Journal of the American Association of Variable Star Observers (Jaavso)*. **43** (1): 38. [Bibcode](/source/Bibcode_(identifier)):[2015JAVSO..43...38M](https://ui.adsabs.harvard.edu/abs/2015JAVSO..43...38M).

v t e Constellation of Centaurus List of stars in Centaurus Centaurus in Chinese astronomy Stars Bayer α A (Rigil Kentaurus) B (Toliman) C (Proxima Centauri) β (Hadar) γ δ ε ζ (Leepwal) η θ (Menkent) ι (Kulou) κ λ μ ν (Heng) ξ1 ξ2 ο1 ο2 π ρ σ τ υ1 υ2 φ χ ψ x1 x2 C3 D E F G H J K M N Q Flamsteed 1 (i) 2 (g) 3 (k) 4 (h) Variable R T V Y RR SV SX BV DY UY V346 V553 V744 V752 V761 (a) V763 (C1) V766 V779 (Krzemiński's star) V803 V810 V816 (Przybylski's Star) V831 V842 V885 V886 V863 V1032 V1369 V1400 V1935 HR 4460 (A) 4466 (C2) 4499 4522 4523 4537 (j) 4546 (B) 4721 4748 (u) 4796 4817 (l) 4831 (w) 4874 (p) 4888 (e) 4889 (n) 4940 (f) 4979 4989 5006 (r) 5041 (m) 5089 (d) 5174 (z) 5222 (y) 5224 5241 5297 5358 (v) 5371 5471 (b) 5485 (c1) 5489 (c2) HD 97413 98176 100453 101581 101930 102117 (Uklun) 103197 107914 108236 109749 110113 113538 113766 114386 114729 115600 116434 (Matza) 117207 117618 (Dofida) 117939 120411 121228 121504 124448 (Popper's Star) 125072 125595 131399 Other 2MASS J1126−5003 2M1207 Gaia BH2 HD 131399 Ab PSR B1259−63 PSR J1311−3430 TOI-763 WASP-15 (Nyamien) WASP-41 WASP-42 WASP-167/KELT-13 Exoplanets 2M1207b b Centauri b HD 101930 b HD 102117 b (Leklsullun) HD 103197 b HD 109749 b HD 113538 b c HD 114386 b HD 114729 b HD 117207 b HD 117618 b (Noifasui) HD 121504 b HIP 65426 b (Najsakopajk) HIP 67522 b NGTS-13b Proxima Centauri b c d WASP-15b (Asye) Star clusters NGC 3766 4230 4507 5281 5286 5316 5460 5617 5662 Other IC 2944 ω Centauri Scorpius–Centaurus association Stock 16 Nebulae NGC 3918 5307 Other Boomerang Nebula Fleming 1 G292.0+1.8 G306.3-0.9 Gum 41 IC 2944 IRAS 13208−6020 RCW 79 RCW 86 Southern Crab Nebula SuWt 2 Galaxies NGC 3557 3568 3749 3783 4444 4603 4622 4650A 4683 4696 4706 4709 4729 4730 4743 4744 4909 4930 4945 4976 5011 A 5026 5064 5082 5090 5091 5102 5114 5121 5128 (Centaurus A) 5161 5206 5253 5266 5291 5398 5408 5419 5483 5516 Other ESO 269-57 ESO 325-4 ESO 383-76 ESO 444-46 Fourcade-Figueroa Object IC 3370 IC 4214 IC 4329A IRAS 13224−3809 J1144−4308 LEDA 677373 PKS 1144−379 PKS 1353−341 PKS 1424−418 Galaxy clusters Abell S740 Centaurus Cluster Shapley Supercluster Astronomical events GW190521 SN 185 SN 1895B (Z) SN 1972E SN 1986G J1407b SN 2019so Category

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