Gamma Doradus variable

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Gamma Doradus variables are variable stars which display variations in luminosity due to non-radial pulsations of their surface. The stars are typically young, early F or late A type main sequence stars, and typical brightness fluctuations are 0.1 magnitudes with periods on the order of one day. This class of variable stars is relatively new, having been first characterized in the second half of the 1990s, and details on the underlying physical cause of the variations remains under investigation.

A light curve for Gamma Doradus, the class prototype, plotted from TESS data GammaDorLightCurve.png
A light curve for Gamma Doradus, the class prototype, plotted from TESS data

The star 9 Aurigae was first noticed to be variable in 1990. However, none of the currently-accepted explanations were adequate: it pulsated too slowly and was outside of the Delta Scuti instability strip, and there was no evidence for any eclipsing material, although Gamma Doradus and HD 96008 were noted to be similar. [2] These three stars, as well as HD 224638, were soon hypothesized to belong to a new class of variable stars in which variability was produced by g-mode pulsations rather than the p-mode pulsations of Delta Scuti variables. [3] HD 224945 and HD 164615 were noticed to be similar as well, while HD 96008 was ruled out on the basis of its more regular period. [4] Eclipses and starspots were soon ruled out as the cause of the Gamma Doradus' variability, [5] and the variability of 9 Aurigae was confirmed to be caused by g-mode pulsations a year later, thus confirming the stars as the prototypes of a new class of variable stars. [6] Over ten more candidates were quickly found, [7] and the discoverers dubbed the group the Gamma Doradus stars, after the brightest member and the first member found to be variable. [8]

List

Designation (name) [9] ConstellationDiscoveryMaximum Apparent magnitude (mV) [10] Minimum Apparent magnitude (mV) [10] Period (days) [9] Spectral classComment
HD 8801 A
(V529 And)
Andromeda Henry & Fekel (2005) [11] 6m.48
(Hipparcos)
6m.51
(Hipparcos)
0.40331A7VmFirst discovered hybrid Gamma Doradus/Delta Scuti variable [11]
V872 Ara [12] Ara Aerts et al. (1998) [12] 6m.37
(Hipparcos)
6m.39
(Hipparcos)
0.4266A9V
9 Aur A Auriga Krisciunas (1993) [3] 4m.935m.501.2582F2VOne of the original stars classified [6]
17 CVn Canes Venatici Henry et al. (2011) [9] 5m.910.8862F0:V Spectroscopic binary; unclear which component is variable
HD 108100
(DD CVn)
Canes Venatici Breger et al. (1996) [13] 7m.150.7541F2V
V350 CMa A Canis Major Eyer & Aerts (2000) [14] 6m.186m.270.7750
10.959
F2VHas two distinct periods
V1026 Cen [12] Centaurus Aerts et al. (1998) [12] 9m.33
(Hipparcos)
9m.38
(Hipparcos)
1.1857A3:m
HD 17163 Cetus Henry et al. (2011) [9] 6m.040.42351F1V
HD 14940 [12]
(EP Cet)
Cetus Aerts et al. (1998) [12] 6m.746m.770.5004F0IV/V
43 Cyg Cygnus Henry et al. (2005) [15] 5m.75
(Hipparcos)
5m.84
(Hipparcos)
0.79955F0V
γ Dor Dorado Krisciunas (1993) [3] 4m.234m.270.7570F1VOne of the original stars classified [6]
8 Dra Draco Aerts et al. (1998) [12] 5m.26
(Hipparcos)
5m.34
(Hipparcos)
0.42450F1VmA7(n)
DI Gru [12] Grus Aerts et al. (1998) [12] 8m.688m.760.8668F3IV
V1325 Her Hercules Kaye et al. (1998) [16] 6m.380.4210F0V
80 Leo Leo Henry & Fekel (2002) [17] 6m.346m.370.45286F3IV
HD 40745
(AC Lep)
Lepus Aerts et al. (1998) [12] 6m.28
(Hipparcos)
6m.30
(Hipparcos)
0.82427F2IV
HD 69682 Lynx Henry et al. (2011) [9] 6m.500.53189A9V
DO Lyn Lynx Kaye et al. (1999) [18] 7m.170.62447F0V
HD 50747 [19] Monoceros Dolez et al. (2009) [19] 5m.454.865
0.956
A4IVTriple star; unknown which component is variable
HD 49434 Monoceros Bruntt et al. (2002) [20] 5m.750.57644F1VHybrid Gamma Doradus/Delta Scuti variable [21]
HD 41547 A Monoceros Henry et al. (2007) [22] 5m.870.81123F4V
α Oph [23]
(Rasalhague)
Ophiuchus Monnier et al. (2010) [23] 2m.080.5850A5IVHybrid Gamma Doradus/Delta Scuti variable
73 Oph A Ophiuchus Fekel & Henry (2003) [24] 6m.11 (B)0.61439F0V+G1V
HD 164615
(V2118 Oph)
Ophiuchus Mantegazza et al. (1994) [4] 7m.027m.090.8117F2IVOne of the original stars classified
V2502 Oph Ophiuchus Aerts et al. (1998) [12] 6m.576m.671.307F2V
HD 38309 Aa Orion Henry et al. (2011) [9] 6m.090.37703F0III:n
NZ Peg Pegasus Henry et al. (2001) [25] 5m.83
(Hipparcos)
5m.86
(Hipparcos)
0.41113F2V
HR 8799
(V342 Peg)
Pegasus Rodriguez & Zerbi (1995) [26] 6m.00
(Hipparcos)
6m.06
(Hipparcos)
0.5053A5V Lambda Boötis star and Vega-like star [27]
V372 Peg Pegasus Kaye et al. (1998) [16] 6m.53 (B)2.594821F3V
39 Peg Pegasus Henry et al. (2005) [15] 6m.436m.530.75574F1V
HD 224638
(BT Psc)
Pisces Krisciunas (1993) [3] 7m.8 (B)1.2323F0VOne of the original stars classified [6]
HD 224945
(BU Psc)
Pisces Mantegazza et al. (1994) [4] 6m.930.5432A9VOne of the original stars classified [6]
QW Pup Puppis Poretti et al. (1997) [28] 4m.474m.500.9584F0IV/V
ι TrA A Triangulum Australe Aerts et al. (1998) [12] 5m.30
(Hipparcos)
5m.42
(Hipparcos)
1.4556F4IV
EE Tuc [12] Tucana Aerts et al. (1998) [12] 6m.72
(Hipparcos)
6m.82
(Hipparcos)
0.6935F2IV
V349 Tel [12] Telescopium Aerts et al. (1998) [12] 7m.60
(Hipparcos)
7m.73
(Hipparcos)
0.6953F0V
KO UMa Ursa Major Kaye et al. (1999) [18] 7m.180.7691F2V
UY UMi [12] Ursa Minor Aerts et al. (1998) [12] 6m.30
(Hipparcos)
6m.38
(Hipparcos)
0.7237F2V
VX UMi Ursa Minor Henry et al. (2001) [25] 6m.48 (B)0.34510A9V
ε1 Lyr B Lyrae Peretto I., Lora S., Peretto G., Furlato G., Barbieri M. - MarSEC (2022) [29] 6m.00 V (0.032) TESS0.415F0V

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<span class="mw-page-title-main">Luminous blue variable</span> Type of star that is luminous, blue, and variable in brightness

Luminous blue variables (LBVs) are massive evolved stars that show unpredictable and sometimes dramatic variations in their spectra and brightness. They are also known as S Doradus variables after S Doradus, one of the brightest stars of the Large Magellanic Cloud. They are extraordinarily rare, with just 20 objects listed in the General Catalogue of Variable Stars as SDor, and a number of these are no longer considered LBVs.

<span class="mw-page-title-main">Delta Scuti variable</span> Subclass of young pulsating star

A Delta Scuti variable is a subclass of young pulsating star. These variables as well as classical cepheids are important standard candles and have been used to establish the distance to the Large Magellanic Cloud, globular clusters, open clusters, and the Galactic Center. The variables follow a period-luminosity relation in certain passbands like other standard candles such as Cepheids. SX Phoenicis variables are generally considered to be a subclass of Delta Scuti variables that contain old stars, and can be found in globular clusters. SX Phe variables also follow a period-luminosity relation. One last sub-class are the pre-main sequence (PMS) Delta Scuti variables.

<span class="mw-page-title-main">Delta Aquilae</span> Binary star system in the constellation Aquila

Delta Aquilae, Latinized from δ Aquilae, is a binary star system in the equatorial constellation of Aquila. It has an apparent visual magnitude of 3.4 and, based upon parallax measurements, is located at a distance of about 50.6 light-years from Earth. It is drifting closer with a radial velocity of −30 km/s. The system is predicted to come to within 25.4 ly (7.8 pc) of the Sun in around 335,000 years.

<span class="mw-page-title-main">9 Aurigae</span> Multiple star system in the constellation Auriga

9 Aurigae is a star system in Auriga (constellation). It has an apparent magnitude of about 5, making it visible to the naked eye in many suburban skies. Parallax estimates made by the Hipparcos spacecraft put it at about 86 light-years from the solar system, although individual Gaia Data Release 3 parallaxes place all three components at 88 light years.

<span class="mw-page-title-main">59 Aurigae</span> Star in the constellation Auriga

59 Aurigae, often abbreviated as 59 Aur, is a star in the constellation Auriga. Its baseline apparent magnitude is 6.1, meaning it can just barely be seen with the naked eye as a dim, yellow-white hued star. Based on parallax measurements, it is located about 483 light-years away from the Sun.

<span class="mw-page-title-main">Instability strip</span> Region of an astronomical diagram

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<span class="mw-page-title-main">HD 182475</span> Star in the constellation Aquila

HD 182475 is a Delta Scuti variable star in the equatorial constellation of Aquila.

<span class="mw-page-title-main">HD 149989</span> Star in the constellation Ara

HD 149989 is a single, variable star in the southern constellation of Ara, located near the western constellation border with Norma. It has the variable star designation V872 Arae, while HD 149989 is the identifier from the Henry Draper Catalogue. This is a dim star near the lower limit of visibility to the naked eye with an apparent visual magnitude that fluctuates around 6.30. It is located at a distance of 167 light years from the Sun based on parallax, and is drifting further away with a radial velocity of 46 km/s.

<span class="mw-page-title-main">V352 Aurigae</span> Star in the constellation Auriga

V352 Aurigae is a variable star in the northern constellation of Auriga. It dimly visible to the naked eye with an apparent visual magnitude that ranges from 6.13 down to 6.18. According to the Bortle scale, it is faintly visible to the naked eye from dark rural skies. The star is located at a distance of approximately 970 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −7 km/s.

<span class="mw-page-title-main">Gamma Doradus</span> Star in the constellation Dorado

Gamma Doradus, Latinized from γ Doradus, is the third-brightest star in the southern constellation of Dorado. It is faintly visible to the naked eye with an apparent visual magnitude of approximately 4.25, and is a variable star, the prototype of the class of Gamma Doradus variables. The star is located at a distance of 67 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +25 km/s. Based on its motion through space, it appears to be a member of the IC 2391 supercluster.

<span class="mw-page-title-main">HD 15082</span> Star in the constellation Andromeda

HD 15082 is a star located roughly 399 light years away in the northern constellation of Andromeda. The star is a Delta Scuti variable and a planetary transit variable. A hot Jupiter type extrasolar planet, named WASP-33b or HD 15082b, orbits this star with an orbital period of 1.22 days. It is the first Delta Scuti variable known to host a planet.

<span class="mw-page-title-main">Gamma Equulei</span> Chemically peculiar A-type main sequence star in the constellation Equuleus

Gamma Equulei, Latinized from γ Equulei, is a double star in the northern constellation of Equuleus. It is located at a distance of around 118 light-years from Earth and is visible to the naked eye with a slightly variable apparent visual magnitude of around 4.7. The star is drifting closer to the Sun with a radial velocity of −16.5 km/s.

<span class="mw-page-title-main">Gamma Coronae Borealis</span> Star in the constellation Corona Borealis

Gamma Coronae Borealis, Latinized from γ Coronae Borealis, is a binary star system in the northern constellation of Corona Borealis. It is visible to the naked eye with an apparent visual magnitude of 3.83. Based upon an annual parallax shift of 22.33 mas as seen from Earth, it is located about 146 light years from the Sun. The system is moving closer to the Sun with a radial velocity of about −15 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.

HD 83446 is a probable astrometric binary star system in the constellation Vela. It is visible to the naked eye with an apparent visual magnitude of 4.34. Based upon an annual parallax shift of 30.5 mas, it is located 107.1 light years from the Sun. The system is moving further away with a heliocentric radial velocity of +18 km/s.

<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">FG Virginis</span> Variable star in the constellation Virgo

FG Virginis is a well-studied variable star in the equatorial constellation of Virgo. It is a dim star, near the lower limit of visibility to the naked eye, with an apparent visual magnitude that ranges from 6.53 down to 6.58. The star is located at a distance of 273.5 light years from the Sun based on parallax measurements, and is drifting further away with a radial velocity of +16 km/s. Because of its position near the ecliptic, it is subject to lunar occultations.

<span class="mw-page-title-main">RR Lyncis</span> Variable star in the constellation Lynx

RR Lyncis is a star system in the northern constellation of Lynx, abbreviated RR Lyn. It is an eclipsing binary of the Algol type; one of the closest in the northern sky at an estimated distance of approximately 263 light years based on parallax measurements. The system is faintly visible to the naked eye with a combined apparent visual magnitude of 5.53. During the primary eclipse the brightness drops to 6.03, while it decreases to magnitude 5.90 with the secondary eclipse. The system is drifting closer to the Sun with a radial velocity of −12 km/s.

<span class="mw-page-title-main">VZ Cancri</span> Variable star in the constellation Cancer

VZ Cancri is a variable star in the constellation Cancer, abbreviated VZ Cnc. It varies in brightness with a period of 0.178364 days, from an apparent visual magnitude of 7.18 down to 7.91, which lies below the typical threshold of visibility for the naked eye. The distance to this star is approximately 724 light years based on parallax measurements, and it is receding from the Sun with a radial velocity of 25 km/s.

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