AE Phoenicis

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AE Phoenicis
AEPheLightCurve.png
A light curve for AE Phoenicis, plotted from TESS data [1]
Observation data
Epoch J2000       Equinox J2000
Constellation Phoenix
Right ascension 01h 32m 32.93s [2]
Declination −49° 31′ 41.29″ [2]
Apparent magnitude  (V)7.56 – 8.25 [3]
Characteristics
Evolutionary stage G0V + G0V [3]
Variable type W UMa [3]
Astrometry
Radial velocity (Rv)21.2 [4]  km/s
Proper motion (μ)RA: +151.48 [2]   mas/yr
Dec.: -53.94 [2]   mas/yr
Parallax (π)19.4490 ± 0.0260  mas [2]
Distance 167.7 ± 0.2  ly
(51.42 ± 0.07  pc)
Absolute magnitude  (MV)4.104 [5]
Details
Age 3.20 ± 1.62 [6]   Gyr
Primary
Mass 1.38 ± 0.06 [7]   M☉
Radius 1.29 ± 0.03 [7]   R☉
Luminosity 1.74+0.30
−0.26 [7]   L☉
Temperature 6,083 [8]   K
Secondary
Mass 0.63 ± 0.02 [7]   M☉
Radius 0.81 ± 0.02 [7]   R☉
Luminosity0.83+0.15
−0.12 [7]   L☉
Temperature 6,310 [8]   K
Other designations
AE Phe, CD−50°410, HD  9528, HIP  7183, SAO  215545 [9]
Database references
SIMBAD data

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. [3] From parallax measurements by the Gaia spacecraft, the system is located at a distance of 168 light-years (51.4 parsecs ) from Earth. [2]

AE Phoenicis is a contact binary of W Ursae Majoris type, composed of two stars so close that their surfaces touch each other. They are separated by 2.70 solar radii [6] and orbit each other with a period of 0.3624 days. [8] They are both classified as G-type main-sequence stars of spectral type G0V. [3] With effective temperatures of 6,083 and 6,310  K, 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] The orbit is circular [10] and is inclined by 86.5° in relation to the plane of the sky. [8]

The combination of photometric and spectroscopic data have allowed the direct determination of the parameters of the stars. The primary component has a mass of 1.38 times the solar mass and a radius of 1.29 times the solar radius, while the secondary has 0.63 times the solar mass and 0.81 times the solar radius. [7] In visible light, the primary star contributes 66.5% of the system's luminosity, while the secondary contributes the rest (33.5%). [8] The light curve shows asymmetries and variations that indicate starspots on the surface of the stars. The reconstruction of the surface of the system by Doppler imaging revealed significant spot coverage in the entire surface of both stars, and the spots seem to evolve in a timescale of days. [4]

Since the stars are in contact, there is considerable mass transfer from the secondary to the primary. It is estimated that the secondary star was initially the more massive star, with 1.69 times the solar mass, while the primary had an initial mass of 1.02 times the solar mass. [6] Observations show the orbital period of the system to be increasing at a rate of 6.17×10−8 days per year, which is direct evidence of this mass transfer. [8] The system was born as a detached binary with an estimated separation of 12.39 solar radii and period of 3.07 days, which by angular momentum loss evolved to the current contact configuration. [6] In the future the two stars will probably merge into a single, fast-rotating star. [11]

Gaia Data Release 2 catalogued a 16.0-magnitude star (G band) with very similar parallax and proper motions to AE Phoenicis. It is separated from AE Phoenicis by 6.0 arcseconds and has a temperature of 4,640 K. [12]

Related Research Articles

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

W Ursae Majoris is the variable star designation for a binary star system in the northern constellation of Ursa Major. It has an apparent visual magnitude of about 7.9, which is too faint to be seen with the naked eye. However, it can be viewed with a small telescope. Parallax measurements place it at a distance of roughly 169 light years (52 parsecs) from Earth.

<span class="mw-page-title-main">UW Canis Majoris</span> Beta Lyrae variable star in the constellation Canis Major

UW Canis Majoris is a star in the constellation Canis Major. It is classified as a Beta Lyrae eclipsing contact binary and given the variable star designation UW Canis Majoris. Its brightness varies from magnitude +4.84 to +5.33 with a period of 4.39 days. Bode had initially labelled it as Tau2 Canis Majoris, but this designation had been dropped by Gould and subsequent authors.

<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">Epsilon Coronae Australis</span> Variable star in the constellation Corona Australis

Epsilon Coronae Australis, is a star system located in the constellation Corona Australis. Varying in brightness between apparent magnitudes of 4.74 to 5 over 14 hours, it is the brightest W Ursae Majoris variable in the night sky.

<span class="mw-page-title-main">SX Corvi</span> Eclipsing binary star in the constellation Corvus

SX Corvi is an eclipsing binary star system in the constellation Corvus, ranging from apparent magnitude 8.99 to 9.25 over 7.6 hours. The system is a contact binary also known as a W Ursae Majoris variable, where the two component stars orbit closely enough to each other for mass to have been transferred between them—in this case the secondary having transferred a large amount of mass to the primary.

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

RR Centauri is a variable star of apparent magnitude maximum +7.29. It is located in the constellation of Centaurus, approximately 320 light years distant from the solar system.

<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.

Phi Phoenicis, Latinized from φ Phoenicis, is a binary star system in the southern constellation of Phoenix. It is faintly visible to the naked eye with an apparent visual magnitude of 5.1. Based upon an annual parallax shift of 10.185 mas as seen from Earth, it is located approximately 320 light years from the Sun. It is moving away with a heliocentric radial velocity of 10.4 km/s.

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

AD Phoenicis is a variable star in the constellation of Phoenix. An eclipsing binary, its apparent magnitude has a maximum of 10.27, dimming to 10.80 during primary and secondary eclipses, which are approximately equal. From parallax measurements by the Gaia spacecraft, the system is located at a distance of 655 light-years from Earth.

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

AI Phoenicis is a variable star in the constellation of Phoenix. An Algol-type eclipsing binary, its apparent magnitude is constant at 8.58 for most of the time, sharply dropping to 9.35 during primary eclipse and to 8.89 during secondary eclipse. The system's variability was discovered by W. Strohmeier in 1972. From parallax measurements by the Gaia spacecraft, the system is located at a distance of 560 light-years from Earth, in agreement with earlier estimates based on its luminosity.

<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">TX Ursae Majoris</span> Eclipsing binary star system in the constellation of Ursa Major

TX Ursae Majoris is an eclipsing binary star system in the northern circumpolar constellation of Ursa Major. With a combined apparent visual magnitude of 6.97, the system is too faint to be readily viewed with the naked eye. The pair orbit each other with a period of 3.063 days in a circular orbit, with their orbital plane aligned close to the line of sight from the Earth. During the primary eclipse, the net brightness decreases by 1.74 magnitudes, while the secondary eclipse results in a drop of just 0.07 magnitude. TX UMa is located at a distance of approximately 780 light years from the Sun based on parallax measurements, but is drifting closer with a mean radial velocity of −13 km/s.

<span class="mw-page-title-main">UX Ursae Majoris</span>

UX Ursae Majoris is an Algol type binary star system in the northern circumpolar constellation of Ursa Major. It is classified as a nova-like variable star similar to DQ Herculis, although no eruptions have been reported. Since its discovery in 1933, this system has been the subject of numerous studies attempting to determine its properties. The combined apparent visual magnitude of UX UMa ranges from 12.57 down to 14.15. The system is located at a distance of approximately 952 light years from the Sun based on parallax, and is drifting further away with a radial velocity of 112 km/s.

<span class="mw-page-title-main">XY Ursae Majoris</span> Eclipsing binary star system in the constellation of Ursa Major

XY Ursae Majoris is a short period binary star system in the northern circumpolar constellation of Ursa Major. It is an eclipsing binary with a baseline apparent visual magnitude of 9.50. The system is located at a distance of 221.5 light years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −10 km/s. It has a relatively high proper motion, traversing the celestial sphere at the angular rate of 0.191″·yr−1.

<span class="mw-page-title-main">EQ Tauri</span>

EQ Tauri is a triple star system in the equatorial constellation of Taurus that includes a contact eclipsing binary. The system is too faint to be viewed with the naked eye, having a baseline apparent visual magnitude of 10.5. During the primary eclipse, the brightness of the system drops to magnitude 11.03, then to 10.97 during the secondary minimum. The secondary eclipse is total. Based on parallax measurements, it is located at a distance of approximately 730 light years from the Sun.

<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">AH Virginis</span> Star in the constellation Virgo

AH Virginis is a contact binary star system in the equatorial constellation of Virgo, abbreviated AH Vir. It is a variable star with a brightness that peaks at an apparent visual magnitude of 9.18, making it too faint to be viewed with the naked eye. The distance to this system is approximately 338 light years based on parallax measurements, and it is drifting further away with a mean radial velocity of 7 km/s. O. J. Eggen in 1969 included this system as a probable member of the Wolf 630 group of co-moving stars.

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

VV Ursae Majoris is a binary star system in the northern circumpolar constellation of Ursa Major, abbreviated VV UMa. It is a variable star system with a brightness that cycles around an apparent visual magnitude of 10.19, making it too faint to be visible to the naked eye. The system is located at a distance of approximately 1,500 light years based on parallax measurements.

<span class="mw-page-title-main">AE Ursae Majoris</span> Variable star in the constellation Ursa Major

AE Ursae Majoris is a star in the northern circumpolar constellation of Ursa Major, abbreviated AE UMa. It is a variable star that ranges in brightness from a peak apparent visual magnitude of 10.86 down to 11.52. The distance to this star is approximately 2,400 light years based on parallax measurements.

<span class="mw-page-title-main">AW Ursae Majoris</span> Variable star in the constellation Ursa Major

AW Ursae Majoris is a binary star system in the northern circumpolar constellation of Ursa Major, abbreviated AW UMa. It is an A-type W Ursae Majoris variable with an apparent visual magnitude of 6.83, which is near the lower limit of visibility to the naked eye. This is an eclipsing binary with the brightness dropping to magnitude 7.13 during the primary eclipse and to 7.08 with the secondary eclipse. Parallax measurements give a distance estimate of 221 light years from the Sun. It is drifting closer to the Sun with a radial velocity of approximately −17 km/s. The system has a high proper motion, traversing the celestial sphere at the rate of 0.216 arc second per annum.

References

  1. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  2. 1 2 3 4 5 6 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 . Gaia DR2 record for this source at VizieR.
  3. 1 2 3 4 5 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 Barnes, J. R.; Lister, T. A.; Hilditch, R. W.; Collier Cameron, A. (2004). "High-resolution Doppler images of the spotted contact binary AE Phe". Monthly Notices of the Royal Astronomical Society. 348 (4): 1321. Bibcode:2004MNRAS.348.1321B. doi: 10.1111/j.1365-2966.2004.07452.x .
  5. ↑ Eker, Z.; Bilir, S.; Yaz, E.; Demircan, O.; Helvaci, M. (2009). "New absolute magnitude calibrations for W Ursa Majoris type binaries". Astronomische Nachrichten. 330 (1): 68. arXiv: 0807.4989 . Bibcode:2009AN....330...68E. doi:10.1002/asna.200811041. S2CID   15071352.
  6. 1 2 3 4 Yıldız, M. (2014). "Origin of W UMa-type contact binaries - age and orbital evolution". Monthly Notices of the Royal Astronomical Society. 437 (1): 185–194. arXiv: 1310.5526 . Bibcode:2014MNRAS.437..185Y. doi:10.1093/mnras/stt1874. S2CID   119121897.
  7. 1 2 3 4 5 6 7 Hilditch, R. W.; King, D. J.; McFarlane, T. M. (1988). "The evolutionary state of contact and near-contact binary stars". Monthly Notices of the Royal Astronomical Society. 231 (2): 341–352. Bibcode:1988MNRAS.231..341H. doi: 10.1093/mnras/231.2.341 .
  8. 1 2 3 4 5 6 7 He, J. -J; Qian, S. -B.; Fernández Lajús, E.; Fariña, C. (2009). "A Charge-Coupled Device Photometric Study of South Hemispheric Contact Binary AE Phoenicis". The Astronomical Journal. 138 (5): 1465. Bibcode:2009AJ....138.1465H. doi: 10.1088/0004-6256/138/5/1465 . hdl: 11336/42802 .
  9. ↑ "AE Phe". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 27 January 2019.
  10. ↑ Duerbeck, H. W. (1978). "The orbit of AE Phe - revisited". Acta Astronomica. 28: 49. Bibcode:1978AcA....28...49D.
  11. ↑ Gazeas, K.; Stȩpień, K. (2008). "Angular momentum and mass evolution of contact binaries". Monthly Notices of the Royal Astronomical Society. 390 (4): 1577. arXiv: 0803.0212 . Bibcode:2008MNRAS.390.1577G. doi: 10.1111/j.1365-2966.2008.13844.x .
  12. ↑ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 . Gaia DR2 record for this source at VizieR.
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