DS Andromedae

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DS Andromedae
NGC 752.png
Red circle.svg
Location of DS Andromedae in NGC 752 (circled)
Observation data
Epoch J2000       Equinox J2000
Constellation Andromeda
Right ascension 01h 57m 46.0561s [1]
Declination +38° 04′ 28.43112″ [1]
Apparent magnitude  (V)10.44 – 10.93 variable [2]
Characteristics
Spectral type F3IV-V + G0V [3]
Apparent magnitude  (B)10.89 [4]
Apparent magnitude  (V)10.52 [4]
Apparent magnitude  (G)10.4555 [1]
Apparent magnitude  (J)9.653 [5]
Apparent magnitude  (H)9.481 [5]
Apparent magnitude  (K)9.407 [5]
Variable type Algol [2]
Astrometry
Radial velocity (Rv)2.5±2.0 [3]  km/s
Proper motion (μ)RA: 10.172±0.082 [1]   mas/yr
Dec.: 11.78±0.08 [1]   mas/yr
Parallax (π)2.1968 ± 0.0404  mas [1]
Distance 1,480 ± 30  ly
(455 ± 8  pc)
Orbit
Period (P)1.0105188 days [2]
Semi-major axis (a)5.77 R☉ [3]
Eccentricity (e)0 [3]
Inclination (i)84.3 [3] °
Periastron epoch (T)HJD 2,436,142.405 [3]
Semi-amplitude (K1)
(primary)		110 [6] km/s
Semi-amplitude (K2)
(secondary)		180 [6] km/s
Details [3]
Primary
Mass 1.58±0.17  M☉
Radius 2.10±0.08  R☉
Luminosity 8.3  L☉
Temperature 6,775  K
Age 2  Gyr
Secondary
Mass 0.94±0.10  M☉
Radius 1.19±0.05  R☉
Luminosity1.6  L☉
Temperature 5,997  K
Age 2  Gyr
Other designations
2MASS J01574604+3804284, BD+37 435, TYC 2816-2203-1
Database references
SIMBAD data

DS Andromedae (often abbreviated to DS And) is an eclipsing binary star in the constellation Andromeda and a member of the open cluster NGC 752. Its maximum apparent visual magnitude is 10.44, but drops down to 10.93 during the main eclipse and to 10.71 during the secondary one.

Contents

System

The primary star has a spectral classification F3IV-V, matching the evidence for a star that is evolving off the main sequence and is expanding its radius. The secondary is thought to be a main sequence star with spectral type G0. It is not visible in the spectrum of DS Andromedae, but the temperature and spectral type can be estimated from the difference in brightness of the two components, determined from the eclipses. The two components are modelled to have apparent magnitudes of 10.62 and 12.47 respectively. [3]

The age of DS Andromedae appears to be very close to the hook at the end of main sequence phase of evolution and has just reached the subgiant branch. Its age can be determined at 2.0±0.2  Gyr from the NGC 752 main sequence turnoff and this allows its physical properties to be accurately calculated. It appears to be not quite filling its roche lobe and no mass transfer has taken place between the two stars; they are evolving as isolated stars. [3]

Variability

The light curve for DS Andromedae, adapted from Milone et al. DSAndLightCurve.png
The light curve for DS Andromedae, adapted from Milone et al.

The light curve of DS Andromedae shows a main eclipse when the secondary star passes in front of the primary, and a secondary eclipse when the opposite occurs. This cycle repeats with a periodicity slightly over one day. Since the system is almost exactly edge-on the secondary eclipse is total, and allows the determination of the spectral type of the secondary component. The primary eclipse is annular as the smaller secondary passes in front of the hotter brighter primary. [3]

It is classified as an Algol variable (detached) star in the General Catalogue of Variable Stars, [2] but is sometimes considered to be a β Lyrae variable (contact). [8]

Related Research Articles

<span class="mw-page-title-main">NGC 752</span> Open cluster in the constellation Andromeda

NGC 752 is an open cluster in the constellation Andromeda. The cluster was discovered by Caroline Herschel in 1783 and cataloged by her brother William Herschel in 1786, although an object that may have been NGC 752 was described by Giovanni Batista Hodierna before 1654.

<span class="mw-page-title-main">WR 22</span> Binary star in the constellation Carina

WR 22, also known as V429 Carinae or HR 4188, is an eclipsing binary star system in the constellation Carina. The system contains a Wolf-Rayet (WR) star that is one of the most massive and most luminous stars known, and is also a bright X-ray source due to colliding winds with a less massive O class companion. Its eclipsing nature and apparent magnitude make it very useful for constraining the properties of luminous hydrogen-rich WR stars.

<span class="mw-page-title-main">HD 63032</span> Binary star system in the constellation Puppis

c Puppis, also known as HD 63032 and HR 3017, is a spectroscopic binary star in the constellation Puppis. Its apparent magnitude is 3.61. Located around 347 parsecs (1,130 ly) distant, the primary is an orange-red bright giant or supergiant of spectral type K2.5Ib-IIa or K5IIa, while the secondary, discovered in 1983, is a blue main-sequence star of spectral type B9V. The system is the brightest member of the open cluster NGC 2451, over two magnitudes brighter than every other star in the cluster. As the turnoff point of the cluster is currently around B7, the parameters of the system fit with cluster membership.

<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

WZ Andromedae is an eclipsing binary star in the constellation Andromeda. Its maximum apparent visual magnitude is 11.6, but drops down to 12.00 during the main eclipse which occurs roughly every 16.7 hours.

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

XZ Andromedae is a binary star in the constellation Andromeda. Its maximum apparent visual magnitude is 9.91, but drops down to 12.45 every 1.357 days. Its variability matches the behaviour of Algol variable stars.

<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">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">BM Andromedae</span> Star in the constellation Andromeda

BM Andromedae is a T Tauri star in the constellation Andromeda. Its apparent visual magnitude has irregular variations between a maximum of 11.63 and a minimum of 14.02.

<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">DX Andromedae</span> Star in the constellation Andromeda

DX Andromedae is a cataclysmic variable star in the constellation Andromeda. It has a typical apparent visual magnitude of 15.5 during the quiescent phase, but becomes brighter during outbursts recurring with a mean cycle length of 330 days, thus is classified as a dwarf nova of the SS Cygni type.

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

FF Andromedae is a spectroscopic binary in the constellation Andromeda. It has a typical apparent visual magnitude of 10.4, but undergoes flare events that can increase its brightness by about a magnitude.

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

KX Andromedae is a spectroscopic binary star in the constellation Andromeda. Its apparent visual magnitude varies between 6.88 and 7.28.

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

KZ Andromedae is a double lined spectroscopic binary in the constellation Andromeda. Its apparent visual magnitude varies between 7.91 and 8.03 during a cycle slightly longer than 3 days.

<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.

<span class="mw-page-title-main">V455 Andromedae</span> Dwarf nova star in the constellation Andromeda

V455 Andromedae is a dwarf nova in the constellation Andromeda. It has a typical apparent visual magnitude of 16.5, but reached a magnitude of 8.5 during the only observed outburst.

<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">WR 133</span> Wolf-Rayet star and spectroscopic binary star in the constellation of Cygnus

WR 133 is a visually moderately bright Wolf-Rayet star. It is a spectroscopic binary system containing a Wolf-Rayet primary and a class O supergiant secondary. It is in the constellation of Cygnus, lying in the sky at the centre of the triangle formed by β and γ Cygni, near η Cygni. It is the brightest member of the sparse open cluster NGC 6871.

References

  1. 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.
  2. 1 2 3 4 DS 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.
  3. 1 2 3 4 5 6 7 8 9 10 Schiller, S. J.; Milone, E. F. (1988). "Photometric and Spectroscopic Analysis of the Eclipsing Binary DS Andromedae- a Member of NGC 752". Astronomical Journal. 95: 1466. Bibcode:1988AJ.....95.1466S. doi: 10.1086/114742 .
  4. 1 2 "DS And". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved October 31, 2018.
  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.
  6. 1 2 Pourbaix, D.; et al. (September 2004), "SB9: The ninth catalogue of spectroscopic binary orbits", Astronomy and Astrophysics, 424 (2): 727–732, arXiv: astro-ph/0406573 , Bibcode:2004A&A...424..727P, doi:10.1051/0004-6361:20041213, S2CID   119387088.
  7. ↑ Milone, E. F.; Schiller, S. J.; Mellergaard Amby, Th.; Frandsen, S. (August 2019). "DS Andromedae: A Detached Eclipsing Double-lined Spectroscopic Binary in the Galactic Cluster NGC 752". The Astronomical Journal. 158 (2): 82. Bibcode:2019AJ....158...82M. doi: 10.3847/1538-3881/ab22ba . S2CID   201262710 . Retrieved 7 October 2021.
  8. ↑ Avvakumova, E. A.; Malkov, O. Yu.; Kniazev, A. Yu. (2013). "Eclipsing variables: Catalogue and classification" (PDF). Astronomische Nachrichten. 334 (8): 860. Bibcode:2013AN....334..860A. doi:10.1002/asna.201311942. hdl: 10995/27061 .
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