AD Andromedae

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AD Andromedae
ADAndLightCurve.png
A visual band light curve of AD Andromedae, from Liakos et al. [1]
Observation data
Epoch J2000       Equinox J2000
Constellation Andromeda
Right ascension 23h 36m 45.00656s [2]
Declination +48° 40′ 15.57327″ [2]
Apparent magnitude  (V)11.2 – 11.82 variable [3]
Characteristics
Spectral type A0V [3]
Apparent magnitude  (B)11.2 [4]
Apparent magnitude  (V)11.0 [4]
Apparent magnitude  (G)11.0304 [2]
Apparent magnitude  (J)10.897 [5]
Apparent magnitude  (H)10.819 [5]
Apparent magnitude  (K)10.769 [5]
B−V color index 0.80 [4]
Variable type β Lyrae [3]
Astrometry
Proper motion (μ)RA: −4.606±0.058 [2]   mas/yr
Dec.: −3.712±0.054 [2]   mas/yr
Parallax (π)0.9179 ± 0.0365  mas [2]
Distance 3,600 ± 100  ly
(1,090 ± 40  pc)
Orbit [4]
Period (P)0.986 days
Semi-major axis (a)7.5 R☉
Inclination (i)82.6°
Periastron epoch (T)HJD 2,439,002.458
Details [4]
Primary
Mass 2.76  M☉
Radius 2.3  R☉
Luminosity 44  L☉
Temperature 9,800  K
Secondary
Mass 2.7  M☉
Radius 2.4  R☉
Luminosity47  L☉
Temperature 9,720  K
Other designations
2MASS J23364500+4840155, BD+47 4207, TYC 3641-151-1, GSC 03641-00151
Database references
SIMBAD data

AD Andromedae (AD And) 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.

Contents

System

The AD Andromedae system consists of two close main sequence stars of spectral type A0V. They orbit so close to each other that they have an ellipsoidal shape induced by their gravitational interaction. [3]

The presence in this system of a third body with a minimum mass of 2.21 M☉ has been proposed; however, it should give a significant contribution to the light emitted by the system, and has not been detected yet. A possible solution is for two unseen, but less massive and luminous, stars orbiting close to each other. [4]

Variability

The orbital plane of the two stars is aligned to our line of sight, so each component eclipses the other when passing in front of it. In AD Andromedae this cycle repeats with a period 20 minutes less than one day. [3]

A cyclic variation of 14.3 years in the orbital period of this binary system has been reported, and this could be an effect of another body orbiting in this system. [4]

Related Research Articles

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

LQ Andromedae is a variable star in the constellation Andromeda. Its maximum apparent visual magnitude is 6.5, placing it at the limit of the visibility to the naked eye. The brightness, however, drops down to 6.66 with a periodic cycle of roughly 7.44 hours.

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

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<span class="mw-page-title-main">XZ Andromedae</span> Binary star in the constellation Andromeda

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<span class="mw-page-title-main">AB Andromedae</span> Binary star in the Andromeda constellation

AB Andromedae is a binary star in the constellation Andromeda. Paul Guthnick and Richard Prager discovered that the star is an eclipsing binary in 1927. Its maximum apparent visual magnitude is 9.49 but shows a variation in brightness down to a magnitude of 10.46 in a periodic cycle of roughly 8 hours. The observed variability is typical of W Ursae Majoris variable stars, so the two stars in this system form a contact binary.

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

BX Andromedae is an eclipsing binary star in the constellation Andromeda. Its maximum apparent visual magnitude is 8.87. Within a cycle of approximately 14.6 hours, the brightness drops down to a magnitude of 9.53 during the main eclipse, and to a magnitude of 9.12 during the secondary one. It is classified as a Beta Lyrae variable.

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

CC Andromedae is a variable star in the constellation Andromeda. It is a pulsating star of the Delta Scuti type, with an apparent visual magnitude that varies between 9.19 and 9.46 with a periodicity of 3 hours.

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

CN Andromedae is an eclipsing binary star in the constellation Andromeda. Its maximum apparent visual magnitude is 9.62 and drops down to a minimum of 10.2 during the main eclipse. It is classified as a Beta Lyrae variable with a period roughly of 0.4628 days.

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

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

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

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<span class="mw-page-title-main">GR Andromedae</span> Variable star in the constellation Andromeda

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

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

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

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

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

QR Andromedae is an eclipsing binary star in the constellation Andromeda. Its maximum apparent visual magnitude is 12.16, but its light curve shows clearly eclipsing events where its brightness can drop to a magnitude of 13.07. This leads to its classification as an Algol variable star.

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

QX Andromedae is an eclipsing binary in the constellation Andromeda. It varies from a maximum apparent visual magnitude of 11.28 to a minimum of 11.50. Since it is impossible to specify the onset time of the eclipses, it is classified as a W Ursae Majoris variable star. It is also observed as an X-ray source and is a member of the open cluster NGC 752.

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References

  1. ↑ Liakos, A.; Niarchos, P.; Budding, E. (March 2012). "A fresh insight into the evolutionary status and third body hypothesis of the eclipsing binaries AD Andromedae, AL Camelopardalis, and V338 Herculis". Astronomy & Astrophysics. 539: A129. Bibcode:2012A&A...539A.129L. doi:10.1051/0004-6361/201117386. S2CID   119274034 . Retrieved 7 October 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 AD And, database entry, Combined General Catalog of Variable Stars (GCVS4.2, 2004 Ed.), N. N. Samus, O. V. Durlevich, et al., CDS ID II/250 Accessed on line 2018-10-17.
  4. 1 2 3 4 5 6 7 Liakos, A.; Niarchos, P.; Budding, E. (March 2012). "A fresh insight into the evolutionary status and third body hypothesis of the eclipsing binaries AD Andromedae, AL Camelopardalis, and V338 Herculis". Astronomy & Astrophysics. 539: II/246. arXiv: 1404.2799 . Bibcode:2012A&A...539A.129L. doi:10.1051/0004-6361/201117386. S2CID   119274034.
  5. 1 2 3 Cutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E.; Fowler, John W.; Gizis, John E.; Howard, Elizabeth V.; Huchra, John P.; Jarrett, Thomas H.; Kopan, Eugene L.; Kirkpatrick, J. Davy; Light, Robert M.; Marsh, Kenneth A.; McCallon, Howard L.; Schneider, Stephen E.; Stiening, Rae; Sykes, Matthew J.; Weinberg, Martin D.; Wheaton, William A.; Wheelock, Sherry L.; Zacarias, N. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". CDS/ADC Collection of Electronic Catalogues. 2246: II/246. Bibcode:2003yCat.2246....0C.
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