SW Andromedae

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SW Andromedae
Observation data
Epoch J2000       Equinox J2000
Constellation Andromeda
Right ascension 00h 23m 43.08963s [1]
Declination 29° 24′ 03.6265″ [1]
Apparent magnitude  (V)9.14 to 10.09 [2]
Characteristics
Spectral type A7III [2]
Apparent magnitude  (U)10.287±0.20 [3] [note 1]
Apparent magnitude  (B)10.097±0.006 [3] [note 1]
Apparent magnitude  (V)9.692±0.006 [3] [note 1]
Apparent magnitude  (Rc)9.433±0.020 [3] [note 1]
Apparent magnitude  (Ic)9.169±0.008 [3] [note 1]
Apparent magnitude  (J)8.757±0.020 [3] [note 1]
Apparent magnitude  (H)8.590±0.013 [3] [note 1]
Apparent magnitude  (Ks)8.511±0.009 [3] [note 1]
Variable type RRab Lyrae [3]
Astrometry
Proper motion (μ)RA: −6.638(29) [1]   mas/yr
Dec.: −18.906(26) [1]   mas/yr
Parallax (π)1.77 ± 0.26  mas [1]
Distance approx. 1,800  ly
(approx. 560  pc)
Absolute magnitude  (MV)0.710 [4]
Details [4]
Mass 0.26±0.04  M☉
Radius 4.51–5.05  R☉
Luminosity 39.8±4  L☉
Temperature 6644  K
Other designations
SW And, BD+28 54, HIP  1878, TYC  1737-1702-1, 2MASS J00234308+2924036 [5]
Database references
SIMBAD data
Phase-folded light curve of the RR Lyrae variable SW Andromedae recorded by NASA's Transiting Exoplanet Survey Satellite (TESS) SW Andromedae TESS folded lightcurve.png
Phase-folded light curve of the RR Lyrae variable SW Andromedae recorded by NASA's Transiting Exoplanet Survey Satellite (TESS)
Light curve of SW AND taken through a J/C V band filter SW AND.png
Light curve of SW AND taken through a J/C V band filter

SW Andromedae is a variable star in the constellation of Andromeda. It is classified as an RR Lyrae star, and varies from an apparent magnitude of 10.09 at minimum brightness to a magnitude of 9.14 at maximum brightness with a period of 0.44226 days. [2] It exhibits the Blazhko effect, and its period is decreasing. [6] [7]

The discovery of this star by Annie Jump Cannon was announced in 1907. 461 photographic plates, spanning the time interval from November 14, 1889 through November 16, 1906 were examined, and an initial period of 0.49932 days was derived. [8] SW Andromedae was given its variable star designation in 1907. [9]

Notes

  1. 1 2 3 4 5 6 7 8 Since SW Andromedae is a variable star these magnitudes are means sampled over the light curve.

Related Research Articles

<span class="mw-page-title-main">RR Lyrae variable</span> Type of variable star

RR Lyrae variables are periodic variable stars, commonly found in globular clusters. They are used as standard candles to measure (extra) galactic distances, assisting with the cosmic distance ladder. This class is named after the prototype and brightest example, RR Lyrae.

<span class="mw-page-title-main">Beta Lyrae</span> Multiple star system in the constellation of Lyra

Beta Lyrae officially named Sheliak, the traditional name of the system, is a multiple star system in the constellation of Lyra. Based on parallax measurements obtained during the Hipparcos mission, it is approximately 960 light-years distant from the Sun.

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

Zeta Andromedae is a star system in the constellation Andromeda. It is approximately 189 light-years from Earth.

<span class="mw-page-title-main">Xi Andromedae</span> K-type giant star in the constellation Andromeda

Xi Andromedae, officially named Adhil, is a solitary star in the northern constellation of Andromeda. It has an apparent magnitude of +4.9. Based on parallax measurements obtained during the Gaia mission, it lies at a distance of roughly 223 light-years from the Sun.

<span class="mw-page-title-main">8 Andromedae</span> Multiple star system in the constellation Andromeda

8 Andromedae, abbreviated 8 And, is a probable triple star system in the northern constellation of Andromeda. 8 Andromedae is the Flamsteed designation. It is visible to the naked eye with an apparent visual magnitude of 4.82. Based upon an annual parallax shift of 5.7 mas, it is located about 570 light years from the Earth. It is moving closer with a heliocentric radial velocity of −8 km/s.

<span class="mw-page-title-main">15 Andromedae</span> Star in the constellation Andromeda

15 Andromedae, abbreviated 15 And, is a single, variable star in the northern constellation of Andromeda. 15 Andromedae is the Flamsteed designation, while its variable star designation is V340 And. Its apparent visual magnitude is 5.55, which indicates it is faintly visible to the naked eye. Its estimated distance from the Earth is 252 light years, and it is moving further away with a heliocentric radial velocity of 13 km/s.

<span class="mw-page-title-main">13 Andromedae</span> Star in the constellation Andromeda

13 Andromedae, abbreviated 13 And, is a single, blue-white hued variable star in the northern constellation of Andromeda. 13 Andromedae is the Flamsteed designation, while it bears the variable star designation V388 Andromedae. With a typical apparent visual magnitude of around 5.75, it is dimly visible to the naked eye under good seeing conditions. The distance to this star can be directly estimated from its annual parallax shift of 10.9 mas, yielding a range of 300 light years. At that distance, its brightness is diminished by an extinction of 0.13 magnitude due to interstellar dust. The star is moving closer to the Earth with a heliocentric radial velocity of −8 km/s.

<span class="mw-page-title-main">S Arae</span> Variable star in the constellation Ara

S Arae (S Ara) is an RR Lyrae-type pulsating variable star in the constellation of Ara. It has an apparent visual magnitude which varies between 9.92 and 11.24 during its 10.85-hour pulsation period, and it exhibits the Blazhko effect.

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

LN Andromedae, also known as HD 217811, HR 8768, is a formerly suspected variable star in the constellation Andromeda. Located approximately 458 parsecs (1,490 ly) away from Earth, it shines with an apparent visual magnitude 6.41, thus it can be seen by the naked eye under very favourable conditions. Its spectral classification is B2V, meaning that it's a hot main sequence star, emitting light approximately with a blackbody spectrum at an effective temperature of 18,090 K.

<span class="mw-page-title-main">V385 Andromedae</span> Star in the constellation Andromeda

V385 Andromedae is a variable star in the constellation Andromeda, about 360 parsecs (1,200 ly) away. It is a red giant over a hundred times larger than the sun. It has an apparent magnitude around 6.4, just about visible to the naked eye in ideal conditions.

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

RR Lyrae is a variable star in the Lyra constellation, figuring in its west near to Cygnus. As the brightest star in its class, it became the eponym for the RR Lyrae variable class of stars and it has been extensively studied by astronomers. RR Lyrae variables serve as important standard candles that are used to measure astronomical distances. The period of pulsation of an RR Lyrae variable depends on its mass, luminosity and temperature, while the difference between the measured luminosity and the actual luminosity allows its distance to be determined via the inverse-square law. Hence, understanding the period-luminosity relation for a local set of such stars allows the distance of more distant stars of this type to be determined.

<span class="mw-page-title-main">RX Andromedae</span> Cataclysmic variable star system in the constellation Andromeda

RX Andromedae is a variable star in the constellation of Andromeda. Although it is classified as a dwarf nova of the Z Camelopardalis (UGZ) type, it has shown low-luminosity periods typical of VY Sculptoris stars. However, for most of the time it varies from an apparent visual magnitude of 15.1 at minimum brightness to a magnitude of 10.2 at maximum brightness, with a period of approximately 13 days.

<span class="mw-page-title-main">64 Eridani</span> Single, yellow-white hued star in the constellation Eridanus

64 Eridani is a single, yellow-white hued star in the constellation Eridanus having variable star designation S Eridani. It is faintly visible to the naked eye with an apparent visual magnitude of 4.77. The annual parallax shift is measured at 12.01 mas, which equates to a distance of about 272 light years. In addition to its proper motion, it is moving closer to the Sun with a radial velocity of around −9 km/s.

<span class="mw-page-title-main">V529 Andromedae</span> Star in the constellation Andromeda

V529 Andromedae, also known as HD 8801, is a variable star in the constellation of Andromeda. It has a 13th magnitude visual companion star 15" away, which is just a distant star on the same line of sight.

<span class="mw-page-title-main">V520 Persei</span> Star in the constellation Perseus

V520 Persei is a blue supergiant member of NGC 869, one of the Perseus Double Cluster open clusters. It is an irregular variable star. At a magnitude of 6.55, V520 Persei is the brightest member in either NGC 869 or NGC 884, although the brighter HD 13994 lies in the foreground along the same line of sight.

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

QV Andromedae is an Alpha2 Canum Venaticorum variable in the constellation Andromeda. Its maximum apparent visual magnitude is 6.6, so it can be seen by the naked eye under very favourable conditions. The brightness varies slightly following a periodic cycle of approximately 5.23 days.

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

AC Andromedae is a variable star in the constellation Andromeda. Its maximum apparent visual magnitude is 10.77, but can be seen fainter down to a magnitude of 11.9.

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

GR Andromedae is a variable star in the constellation Andromeda. Its apparent visual magnitude varies between 6.87 and 6.95 in a cycle of 518.2 days. It is classified as an α2 Canum Venaticorum variable.

<span class="mw-page-title-main">DY Pegasi</span> Star in the constellation Pegasus

DY Pegasi, abbreviated DY Peg, is a binary star system in the northern constellation of Pegasus. It is a well-studied SX Phoenicis variable star with a brightness that ranges from an apparent visual magnitude of 9.95 down to 10.62 with a period of 1.75 hours. This system is much too faint to be seen with the naked eye, but can be viewed with large binoculars or a telescope. Based on its high space motion and low abundances of heavier elements, it is a population II star system.

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

TU Ursae Majoris is a variable star in the northern circumpolar constellation of Ursa Major. It is classified as a Bailey-type 'ab' RR Lyrae variable with a period of 0.557648 days that ranges in brightness from apparent visual magnitude of 9.26 down to 10.24. The distance to this star is approximately 2,090 light years based on parallax measurements. It is located near the north galactic pole at a distance that indicates this is a member of the galactic halo.

References

  1. 1 2 3 4 5 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.
  2. 1 2 3 SW 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 2014-07-02.
  3. 1 2 3 4 5 6 7 8 9 Monson, Andrew J.; et al. (2017). "Standard Galactic Field RR Lyrae. I. Optical to Mid-infrared Phased Photometry". The Astronomical Journal. 153 (3). 96. arXiv: 1703.01520 . Bibcode:2017AJ....153...96M. doi: 10.3847/1538-3881/153/3/96 . S2CID   59322123.
  4. 1 2 Barcza, S.; Benkő, J. M. (2014). "Fundamental parameters of RR Lyrae stars from multicolour photometry and Kurucz atmospheric models – III. SW And, DH Peg, CU Com and DY Peg". Monthly Notices of the Royal Astronomical Society. 442 (2): 1863–1876. arXiv: 1405.4184 . Bibcode:2014MNRAS.442.1863B. doi: 10.1093/mnras/stu978 . S2CID   119182612.
  5. ↑ "V* SW And". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2018-04-21.
  6. ↑ McNamara, D. H.; Feltz, K. A., Jr. (October 1977). "A photometric study of SW Andromedae". Publications of the Astronomical Society of the Pacific. 89: 699–703. Bibcode:1977PASP...89..699M. doi:10.1086/130212 . Retrieved 5 November 2024.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  7. ↑ Skarka, M. (February 2014). "Bright Blazhko RRab Lyrae stars observed by ASAS and the SuperWASP surveys" (PDF). Astronomy & Astrophysics. 562: A90. arXiv: 1402.3111 . Bibcode:2014A&A...562A..90S. doi:10.1051/0004-6361/201322491 . Retrieved 5 November 2024.
  8. ↑ Fleming, Williamina; Cannon, Annie J.; Wells, L. D.; Pickering, Edward C. (January 1907). "Stars Having Peculiar Spectra. 18 New Variable Stars". Harvard College Observatory Circular. 124: 1–4. Bibcode:1907HarCi.124....1F . Retrieved 5 November 2024.
  9. ↑ Duné; Hartwig; Müller (November 1907). "Benennung von neu entdeckten veränderlichen Sternen". Astronomische Nachrichten. 176 (12): 181–194. Bibcode:1907AN....176..181.. doi:10.1002/asna.19071761202 . Retrieved 5 November 2024.


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