V346 Centauri

Last updated
V346 Centauri
V346CenLightCurve.png
A blue band light curve for V346 Centauri, adapted from van Genderen and Sterken (2007) [1]
Observation data
Epoch J2000       Equinox J2000
Constellation Centaurus
Right ascension 11h 42m 49.67s [2]
Declination −62° 26′ 05.40″ [2]
Apparent magnitude  (V)8.50 – 8.77 [3]
(8.72 + 10.38) [4]
Characteristics
Spectral type B0.5IV + B2V [5]
Variable type eclipsing binary (Algol) [3]
Astrometry
Radial velocity (Rv)−6.4 km/s [2]  km/s
Proper motion (μ)RA: −6.236 [6]   mas/yr
Dec.: 0.758 [6]   mas/yr
Parallax (π)0.4380 ± 0.0261  mas [6]
Distance 7,400 ± 400  ly
(2,300 ± 100  pc)
Absolute magnitude  (MV)−3.91 + −2.14 [4]
Absolute bolometric
magnitude  (Mbol)		−6.565 + −4.764 [5]
Orbit [5]
Period (P)6.321843 days
Semi-major axis (a)39.358±0.094 R☉
Eccentricity (e)0.287
Inclination (i)84.423±0.017°
Semi-amplitude (K1)
(primary)		136.46±0.43 km/s
Semi-amplitude (K2)
(secondary)		191.65±1.29 km/s
Details [5]
Age 10+6
−4 [4]   Myr
Primary
Mass 12.00±0.07  M☉
Radius 8.248±0.014  R☉
Luminosity 33,574  L☉
Surface gravity (log g)3.684  cgs
Temperature 27,141  K
Rotational velocity (v sin i)160.0 km/s
Secondary
Mass 8.47±0.10  M☉
Radius 4.118±0.015  R☉
Luminosity6,391  L☉
Surface gravity (log g)4.137  cgs
Temperature 25,376±18  K
Rotational velocity (v sin i)92.7 km/s
Other designations
V346 Cen, CD−61°3158, HD  101837 [2]
Database references
SIMBAD data

V346 Centauri is a variable star in the constellation Centaurus. An Algol-type eclipsing binary, its apparent magnitude has a maximum of 8.50, dropping to 8.77 during primary eclipse and to 8.72 during secondary eclipse, [3] the latter being a total eclipse. From parallax measurements by the Gaia spacecraft, the system is located at a distance of about 2300  parsecs (7400  light-years), [6] which is consistent with earlier estimates, based on its luminosity, of 2380 parsecs. [4] The system is a confirmed member of the open cluster Stock 14, which contains many other young OB stars. [4]

Both stars in the system are hot B-type stars, with spectral types of B0.5IV and B2V. [5] The primary star shows signs of being evolved, while the secondary is still in the main sequence. [4] In 1936, William O'Leary and Daniel Joseph Kelly O'Connell announced their discovery that the star, then known as CPD-61° 2551, is a eclipsing binary star. [7] It was given its variable star designation, V346 Centauri, later that same year. [8] Due to the eclipsing and double-lined nature of the system, the physical elements of the stars can be determined with high precision. The primary star has a mass of 12 times the solar mass, radius of 8.3 times the solar radius, and an effective temperature of about 27,000  K. The secondary star is smaller and cooler, with 8.5 times the solar mass, 4.1 times the solar radius, and temperature of 25,000 K. In visible light, the primary contributes about 84% of the system's luminosity, while the secondary contributes the rest (16%). There is no evidence in the spectrum or the light curve for a third star in the system. [5]

The average separation between the stars is about 39 solar radii. The orbit of the system has a moderate eccentricity of 0.287 and is inclined by 84.4° in relation to the plane of the sky. It displays apsidal precession with a period of 306±4 years, which means that the argument of periapsis has a cyclical variation with this period. The times of minimum light of the system indicate that the orbital period changed suddenly around the year 1965, decreasing from 6.322123 to 6.321843 days (a decrease of 24 seconds). The reason for this is unknown. [5]

Related Research Articles

<span class="mw-page-title-main">9 Andromedae</span> Star in the constellation Andromeda

9 Andromedae, abbreviated 9 And by convention, is a variable binary star system in the northern constellation Andromeda. 9 Andromedae is the Flamsteed designation, while it bears the variable star designation AN Andromedae, or AN And. The maximum apparent visual magnitude of the system is 5.98, which places it near the lower limit of visibility to the human eye. Based upon an annual parallax shift of 7.1 mas, it is located 460 light years from the Earth.

<span class="mw-page-title-main">31 Camelopardalis</span> Binary star system in the constellation Camelopardalis

31 Camelopardalis is a binary star system in the northern circumpolar constellation of Camelopardalis. It is visible to the naked eye as a dim point of light with a peak apparent visual magnitude of +5.12. Parallax measurements provide a distance estimate of approximately 460 light years away from the Sun, and the system is drifting closer to the Earth with a radial velocity of −3 km/s.

3 Centauri is a triple star system in the southern constellation of Centaurus, located approximately 300 light years from the Sun. It is visible to the naked eye as a faint, blue-white hued star with a combined apparent visual magnitude of 4.32. As of 2017, the two visible components had an angular separation of 7.851″ along a position angle of 106°. The system has the Bayer designation k Centauri; 3 Centauri is the Flamsteed designation. It was a suspected eclipsing binary with a variable star designation V983 Centauri, however the AAVSO website lists it as non-variable, formerly suspected to be variable.

<span class="mw-page-title-main">S Antliae</span> Star in the constellation Antlia

S Antliae is a W Ursae Majoris-type eclipsing binary star in Antlia.

<span class="mw-page-title-main">DV Aquarii</span> Binary star in the constellation Aquarius

DV Aquarii is a binary star system in the zodiac constellation of Aquarius, near the border with Capricornus. It has a peak apparent visual magnitude of 5.89, which is bright enough to be visible to the naked eye. The distance can be estimated from its annual parallax shift of 11.2 mas, yielding a separation of 291 light years.

<span class="mw-page-title-main">IU Aurigae</span> Triple star system in the constellation Auriga

IU Aurigae is a triple star system in the constellation Auriga, consisting of an eclipsing binary pair orbiting a third component with a period of 335 years. This system is too faint to be viewed with the naked eye, having a peak apparent visual magnitude of 8.19.

<span class="mw-page-title-main">68 Herculis</span> Triple star system in the constellation Hercules

68 Herculis is a triple star system located around 950 light-years away from the Sun in the northern constellation of Hercules. In the astronomical community it is often referred to by its Bayer designation of u Herculis, while 68 Herculis is the Flamsteed designation. The system is visible to the naked eye as a faint, blue-white-hued point of light with a peak apparent visual magnitude of 4.80. It is approaching the Earth with a heliocentric radial velocity of −17 km/s.

<span class="mw-page-title-main">RR Centauri</span> Star in the constellation Centaurus

RR Centauri is a variable star with an apparent magnitude of +7.29 when it is at its brightest. It is located in the constellation of Centaurus, approximately 320 light years distant from the solar system.

Psi<sup>2</sup> Orionis Spectroscopic binary system in the constellation of Orion

Psi2 Orionis a binary star system in the equatorial constellation of Orion. It has an apparent visual magnitude of 4.6, indicating that it is visible to the naked eye. Based upon an annual parallax shift of 2.87 mass, it is roughly 1,100 light years distant from the Sun.

<span class="mw-page-title-main">65 Ursae Majoris</span> Star system in the constellation Ursa Major

65 Ursae Majoris, abbreviated as 65 UMa, is a star system in the constellation of Ursa Major. With a combined apparent magnitude of about 6.5, it is at the limit of human eyesight and is just barely visible to the naked eye in ideal conditions. It is about 760 light years away from Earth.

<span class="mw-page-title-main">SV Centauri</span> Star in the constellation Centaurus

SV Centauri is a variable star in the constellation Centaurus. An eclipsing binary, its visual apparent magnitude has a maximum of 8.71, fading to 9.98 during primary eclipse and 9.42 during secondary eclipse. From its brightness, it's estimated to be around 6,000 light-years away from Earth. Parallax measurements from Gaia Data Release 2 yield a similar distance of around 2,100 pc. Henrietta Leavitt announced the discovery of this variable star, in 1906, when it was called CPD-59° 3809. It was given its variable star designation, SV Centauri, in 1907.

<span class="mw-page-title-main">SX Centauri</span> Supergiant variable star in the constellation Centaurus

SX Centauri is a variable star in the constellation Centaurus. An RV Tauri variable, its light curve alternates between deep and shallow minima, varying its apparent magnitude from 9.1 to 12.4. From the period-luminosity relationship, it is estimated to be around 1.6 kpc from Earth. Gaia Data Release 2 gives a parallax of 0.2175 mas, corresponding to distance of about 4,600 pc. Henrietta Leavitt announced the discovery of this variable star, in 1906, when it was called CPD-48° 4730. It was given its variable star designation, SX Centauri, in 1907.

<span class="mw-page-title-main">TW Andromedae</span> Star in the constellation Andromeda

TW Andromedae is an eclipsing binary star, classified also as an Algol variable star, in the constellation Andromeda. Its brightness varies with a period of 4.12 days, and has a typical brightness of magnitude 8.98 but decreasing down to a magnitude of 11.04 during the main eclipse.

<span class="mw-page-title-main">AD Andromedae</span> Eclipsing binary star in the constellation Andromeda

AD Andromedae is an eclipsing binary in the constellation Andromeda. Its maximum apparent visual magnitude is 11.2, but it shows a decrease of 0.62 magnitudes during the main eclipse and 0.58 during the secondary one. It is classified as a Beta Lyrae variable star with a period of almost one day.

<span class="mw-page-title-main">AE Phoenicis</span> Star in the constellation Phoenix

AE Phoenicis is a variable star in the constellation of Phoenix. An eclipsing binary, its apparent magnitude has a maximum of 7.56, dimming to 8.25 during primary eclipse and 8.19 during secondary eclipse. From parallax measurements by the Gaia spacecraft, the system is located at a distance of 168 light-years from Earth.

<span class="mw-page-title-main">V752 Centauri</span> Star in the constellation Centaurus

V752 Centauri is multiple star system and variable star in the constellation of Centaurus. An eclipsing binary, its apparent magnitude has a maximum of 9.10, dimming to 9.66 during primary eclipse and 9.61 during secondary eclipse. Its variability was discovered by Howard Bond in 1970. From parallax measurements by the Gaia spacecraft, the system is located at a distance of 410 light-years from Earth.

<span class="mw-page-title-main">AO Serpentis</span> Star in the constellation Serpens

AO Serpentis is an eclipsing binary star system in the Serpens Caput segment of the Serpens constellation. It is invisible to the naked eye with a typical apparent visual magnitude of 11.04. Variable star observers record a peak magnitude of 10.7, dropping to 12.0 during the primary eclipse and 10.8 from the secondary eclipse. The distance to this system is approximately 1,450 light years based on parallax measurements.

<span class="mw-page-title-main">AG Virginis</span> Eclipsing binary star in the constellation Virgo

AG Virginis is an eclipsing binary star system in the equatorial constellation of Virgo. With a maximum apparent visual magnitude of 8.51 it is too faint to be visible to the naked eye. The system is located at a distance of approximately 820 light years from the Sun based on parallax measurements.

<span class="mw-page-title-main">BH Virginis</span> Eclipsing binary star in the constellation Virgo

BH Virginis is a binary star system in the equatorial constellation of Virgo. With a typical apparent visual magnitude of 9.6, it is too faint to be visible to the naked eye. Based on parallax measurements, it is located at a distance of approximately 488 light years from the Sun. The system is drifting closer with a net radial velocity of −23 km/s.

<span class="mw-page-title-main">RY Persei</span> Star in the constellation Perseus

RY Persei is a variable star in the northern constellation of Perseus, abbreviated RY Per. It is an Algol variable with a period of 6.8635663 days, which indicates this is an eclipsing binary star system with an orbital plane oriented close to the line of sight from the Earth. The system has a maximum apparent visual magnitude of 8.50, which drops down to magnitude 10.25 during the eclipse of the primary component, then to 8.65 with the secondary eclipse. Based on parallax measurements, this system is located at a distance of approximately 2,960 light years from the Sun, but is drifting closer with a radial velocity of −12 km/s.

References

  1. ↑ van Genderen, A. M.; Sterken, C. (July 2007). "Orbital effects on the light curves of eta Car, BP Cru, and Other Eccentric Binaries". Information Bulletin on Variable Stars. 5782: 1. Bibcode:2007IBVS.5782....1V . Retrieved 16 June 2022.
  2. 1 2 3 4 "V346 Cen". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 13 April 2022.
  3. 1 2 3 Samus', N. N; Kazarovets, E. V; Durlevich, O. V; Kireeva, N. N; Pastukhova, E. N (2017). "General catalogue of variable stars: Version GCVS 5.1". Astronomy Reports. 61 (1): 80. Bibcode:2017ARep...61...80S. doi:10.1134/S1063772917010085. S2CID   125853869.
  4. 1 2 3 4 5 6 Gimenez, A.; Clausen, J. V.; Andersen, J. (1986). "Four-colour photometry of eclipsing binaries XXIA. Photometric analysis and apsidal motion study of V346 Centauri". Astronomy and Astrophysics. 160: 310. Bibcode:1986A&A...160..310G.
  5. 1 2 3 4 5 6 7 Mayer, Pavel; Harmanec, Petr; Wolf, Marek; Nemravová, Jana; Prša, Andrej; Frémat, Yves; Zejda, Miloslav; Liška, Jiři; Juryšek, Jakub; Hoňková, Kateřina; Mašek, Martin (2016). "V346 Centauri: Early-type eclipsing binary with apsidal motion and abrupt change of orbital period". Astronomy and Astrophysics. 591: A129. Bibcode:2016A&A...591A.129M. doi: 10.1051/0004-6361/201628655 .
  6. 1 2 3 4 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.
  7. ↑ O'Leary, W.; O'Connell, D. (July 1936). "New Southern Variables". Astronomische Nachrichten. 259: 399. Bibcode:1936AN....259..399O. doi:10.1002/asna.19362592405 . Retrieved 15 January 2025.
  8. ↑ Guthnick, P.; Prager, R. (October 1936). "Benennung von veränderlichen Sternen (in German)". Astronomische Nachrichten. 260: 393–412. Bibcode:1936AN....260..393G. doi:10.1002/asna.19362602202 . Retrieved 15 January 2025.
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.