R Carinae

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R Carinae
RCarLightCurve.png
The visual band light curve of R Carinae, from AAVSO data [1]
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Carina
Right ascension 09h 32m 14.59610s [2]
Declination −62° 47′ 20.0026″ [2]
Apparent magnitude  (V)3.9 - 10.5 [3]
Characteristics
Evolutionary stage AGB [4]
Spectral type M6/7pe [5]
B−V color index 0.906±0.009 [6]
Variable type Mira [3]
Astrometry
Radial velocity (Rv)+28.1±1.0 [6]  km/s
Proper motion (μ)RA: −36.291  mas/yr [2]
Dec.: +19.535  mas/yr [2]
Parallax (π)5.5018 ± 0.3345  mas [2]
Distance 590 ± 40  ly
(180 ± 10  pc)
Absolute magnitude  (MV)1.48 [6] (at mv = 7.43)
Details
Mass 0.87+0.47
−0.31 [4]   M☉
Radius 400±2 (2013) [7] R☉
581–652 (2018) [8] R☉
540±50 (2020) [7]   R☉
Luminosity 4,571+1,331
−1,031 [4]   L☉
Temperature 2,800 [9]   K
Other designations
R Car, CD−62°396, GC  13192, HD  82901, HIP  46806, HR  3816, SAO  250614, CCDM J09322-6247, WDS J09322-6247AB [10]
Database references
SIMBAD data

R Carinae is a double star in the southern constellation of Carina. The brighter component is a variable star that can be viewed with the naked eye at peak brightness, [11] but is usually too faint to be seen without a telescope, having an apparent visual magnitude that fluctuates around 7.43. [6] This star is located at a distance of approximately 600  light years from the Sun based on parallax, [2] and is drifting further away with a radial velocity of +28 km/s. [6]

Benjamin Apthorp Gould discovered the variable star, in 1871. It appeared with its variable star designation in Annie Jump Cannon's 1907 work, Second Catalogue of Variable Stars. [12] The main component is an aging red giant star on the asymptotic giant branch [4] with a stellar classification of M6/7pe. [5] It is classified as a pulsating Mira type variable star and its visual brightness varies with an average amplitude of 4.25 magnitudes over a period of 303.99±1.08 d. Its average maximum visual magnitude is 5.05±0.45, [11] but the brightest observed maximum was magnitude 3.9. [3] The pulsations make its size change, in 2014, it was 400 times larger than the Sun, while in 2020 it was 540 times larger. [7] This star is surrounded by a dusty shell, with properties that are consistent with iron-poor silicates or corundum, extending from around three stellar radii outward. [13]

The companion is a magnitude 11.30 star at an angular separation of 2.10″ along a position angle of 132° from the main star, as of 2015. [14]

Related Research Articles

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

Mira variables are a class of pulsating stars characterized by very red colours, pulsation periods longer than 100 days, and amplitudes greater than one magnitude in infrared and 2.5 magnitude at visual wavelengths. They are red giants in the very late stages of stellar evolution, on the asymptotic giant branch (AGB), that will expel their outer envelopes as planetary nebulae and become white dwarfs within a few million years.

<span class="mw-page-title-main">Eta Aquilae</span> Multiple star in the constellation Aquila

Eta Aquilae is a multiple star in the equatorial constellation of Aquila, the eagle. It was once part of the former constellation Antinous. Its apparent visual magnitude varies between 3.49 and 4.3, making it one of the brighter members of Aquila. Based upon parallax measurements made by the Gaia spacecraft on its third data release (DR3), this star is located at a distance of roughly 272 parsecs. The primary component is a Classical Cepheid variable.

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

RT Aurigae is a yellow supergiant variable star in the constellation Auriga, about 1,500 light years from Earth. Although its brightness is variable, it as consistently visible to the naked eye under good observing conditions.

L<sub>2</sub> Puppis Star in the constellation Puppis

L2 Puppis (also known as HD 56096) is a giant star in the constellation of Puppis and is located between the bright stars Canopus and Sirius. It is a semi-regular pulsating star, and is intermittently visible to the naked eye.

<span class="mw-page-title-main">R Aquilae</span> Red giant star in the constellation Aquila

R Aquilae is a variable star in the equatorial constellation of Aquila. It is located approximately 760 light years distant from the Sun and is drifting further away with a radial velocity of 35 km/s. This is a thermally-pulsating Mira variable that ranges in brightness from magnitude 5.3 down to 12.0 with a period of 269.84 days. The period was over 300 days when first observed, and has declined steadily since – decreasing from 320 in 1915 down to 264 in 2010, at an average rate of 0.4 days per year. The amplitude of the variation has also decreased by about a magnitude since discovery. The peak magnitude is bright enough for the star to be visible to the naked eye as a dim, red-hued star.

<span class="mw-page-title-main">R Canum Venaticorum</span> Star in the constellation Canes Venatici

R Canum Venaticorum is a Mira variable star in the constellation Canes Venatici. It ranges between magnitudes 6.5 and 12.9 over a period of approximately 329 days. It is too faint to be seen with the naked eye, but when it is near its maximum brightness, it can be seen with binoculars.

<span class="mw-page-title-main">HD 155035</span> Star in the constellation Ara

HD 155035 is a star in the constellation Ara, the Altar. It is located at a distance of approximately 1,450 light-years from Earth and has an apparent visual magnitude of 5.92, making it is faintly visible to the naked eye. This is a red giant star with a stellar classification of M1.5 III.

<span class="mw-page-title-main">HD 27245</span> Star in the constellation Camelopardalis

HD 27245, also known as HR 1335 or rarely 25 H. Camelopardalis is a solitary red-hued star located in the northern circumpolar constellation Camelopardalis. It has an apparent magnitude of 5.4, making it faintly visible to the naked eye. Gaia DR3 Parallax measurements place it approximately 607 light years away from it the Solar System and is drifting further away with a heliocentric radial velocity of 25.2 km/s. At its current distance, HD 27245's brightness is diminished by 0.36 magnitudes due to extinction from interstellar dust. It has an absolute magnitude of −0.27.

Omega<sup>1</sup> Cygni B-type subgiant star in the constellation Cygnus

Omega1 Cygni, Latinized from ω1 Cygni, is the Bayer designation for a solitary star in the northern constellation of Cygnus. It is visible to the naked eye with an apparent visual magnitude of 4.94. Based upon an annual parallax shift of 2.59 mas, it is estimated to lie roughly 1,260 light years from the Sun. Relative to its neighbors, this star has a peculiar velocity of 25.7±2.2 km/s.

<span class="mw-page-title-main">Sigma Ophiuchi</span> Star in the constellation Ophiuchus

Sigma Ophiuchi, Latinized from σ Ophiuchi, is a single, orange-hued star in the equatorial constellation Ophiuchus. Its apparent visual magnitude is 4.31, which is bright enough to be faintly visible to the naked eye. The annual parallax shift of 3.62 mas as seen from Earth provides a distance estimate of roughly 900 light years. It is moving closer to the Sun with a radial velocity of −28 km/s.

<span class="mw-page-title-main">ET Virginis</span> Evolved red giant star in the constellation Virgo

ET Virginis is a single, red-hued star in the equatorial constellation of Virgo. It can be viewed with the naked eye, having an apparent visual magnitude of 4.91. Based upon an annual parallax shift of 5.9 mas, it is located 560 light years away. It is moving further from the Earth with a heliocentric radial velocity of +18.6 km/s, having come within 177 ly of the Sun around 6.3 million years ago.

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

R Cancri is a Mira variable in the constellation Cancer. Located approximately 250 parsecs (830 ly) distant, it varies between magnitudes 6.07 and 12.3 over a period of approximately 357 days. At its brightest, it is very faintly visible to the naked eye.

<span class="mw-page-title-main">TW Horologii</span> Star in the constellation Horologium

TW Horologii is a carbon star and semiregular variable in the southern constellation of Horologium, near the eastern constellation border with Reticulum. It has a ruddy hue and, with an apparent visual magnitude that ranges from 5.52 down to 5.95, is visible to the naked eye and one of the brightest carbon stars. Based on parallax measurements, it is located at a distance of approximately 1,370 light years from the Sun. It is drifting further away with a radial velocity of +14 km/s. In the past this star has been considered a member of the open cluster NGC 1252, but this now seems unlikely.

<span class="mw-page-title-main">W Aquilae</span> Variable star in the constellation Aquila

W Aquilae is a variable star in the constellation of Aquila. It is a type of evolved star known as an S-type star. Due to its relatively close distance of 1,200 light-years and equatorial location, it is easy to observe and heavily studied.

<span class="mw-page-title-main">S Cassiopeiae</span> Star in the constellation Cassiopeia

S Cassiopeiae is a Mira variable and S-type star in the constellation Cassiopeia. It is an unusually cool star, rapidly losing mass and surrounded by dense gas and dust producing masers.

<span class="mw-page-title-main">Rho Phoenicis</span> Variable star in the constellation Phoenix

Rho Phoenicis is a variable star in the constellation of Phoenix. From parallax measurements by the Gaia spacecraft, it is located at a distance of 245 light-years from Earth.

<span class="mw-page-title-main">R Fornacis</span> Variable star in the constellation Fornax

R Fornacis is a Mira variable and carbon star located in the constellation Fornax. It is around 1,800 light years away based on parallax measurements.

<span class="mw-page-title-main">HR 3831</span> Binary star system in the constellation Vela

HR 3831, also known as HD 83368, is a binary star system in the southern constellation of Vela at a distance of 233 light years. This object is barely visible to the naked eye as a dim, blue star with an apparent visual magnitude of 6.232. It is approaching the Earth with a heliocentric radial velocity of 4.0±0.3 km/s.

<span class="mw-page-title-main">SZ Tauri</span> Variable star in Taurus

SZ Tauri is a variable star in the equatorial constellation of Taurus. The brightness of this star varies from an apparent visual magnitude of 6.39 down to 6.69 with a period of 3.149 days, which is near the lower limit of visibility to the naked eye. The distance to this star is approximately 2,070 light years based on parallax measurements. There is some indication this may be a binary system, but the evidence is inconclusive.

<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.

References

  1. ↑ "Download Data". aavso.org. AAVSO. Retrieved 1 October 2021.
  2. 1 2 3 4 5 6 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211 . Bibcode:2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940 . S2CID   244398875. Gaia DR3 record for this source at VizieR.
  3. 1 2 3 Samus, N. N.; et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, 5.1, 61 (1): 80–88, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085, S2CID   125853869.
  4. 1 2 3 4 Takeuti, Mine; et al. (2013), "A Method to Estimate the Masses of Asymptotic Giant Branch Variable Stars", Publications of the Astronomical Society of Japan, 65 (3): 60, Bibcode:2013PASJ...65...60T, doi: 10.1093/pasj/65.3.60 .
  5. 1 2 Houk, Nancy; Cowley, A. P. (1979), Michigan catalogue of two-dimensional spectral types for the HD stars, vol. 1, Ann Arbor, Michigan: Dept. of Astronomy, University of Michigan, Bibcode:1978mcts.book.....H.
  6. 1 2 3 4 5 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv: 1108.4971 , Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID   119257644.
  7. 1 2 3 Rosales-Guzmán, A.; Sanchez-Bermudez, J.; Paladini, C.; Freytag, B.; Wittkowski, M.; Alberdi, A.; Baron, F.; Berger, J.-P.; Chiavassa, A.; Höfner, S.; Jorissen, A.; Kervella, P.; Bouquin, J.-B. Le; Marigo, P.; Montargès, M. (2024-08-01), "A new dimension in the variability of AGB stars: Convection patterns size changes with pulsation", Astronomy & Astrophysics , 688: A124, arXiv: 2405.10164 , doi:10.1051/0004-6361/202349112, ISSN   0004-6361
  8. ↑ Rosales-Guzmán, A.; Sanchez-Bermudez, J.; Paladini, C.; Alberdi, A.; Brandner, W.; Cannon, E.; González-Torá, G.; Haubois, X.; Henning, Th; Kervella, P.; Montarges, M.; Perrin, G.; Schödel, R.; Wittkowski, M. (2023-06-01). "Imaging the innermost gaseous layers of the Mira star R Car with GRAVITY-VLTI". Astronomy & Astrophysics. 674: A62. doi:10.1051/0004-6361/202245370. ISSN   0004-6361.
  9. ↑ McDonald, I.; Zijlstra, A. A.; Boyer, M. L. (2012), "Fundamental parameters and infrared excesses of Hipparcos stars", Monthly Notices of the Royal Astronomical Society, 427 (1): 343, arXiv: 1208.2037 , Bibcode:2012MNRAS.427..343M, doi: 10.1111/j.1365-2966.2012.21873.x , S2CID   118665352.
  10. ↑ "R Car". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2020-01-30.
  11. 1 2 Vogt, N.; et al. (2016), "Determination of Pulsation Periods and Other Parameters of 2875 Stars Classified As Mira in the All Sky Automated Survey (Asas)", The Astrophysical Journal Supplement Series, 227 (1): 6, arXiv: 1609.05246 , Bibcode:2016ApJS..227....6V, doi: 10.3847/0067-0049/227/1/6 , S2CID   119295645.
  12. ↑ Cannon, Annie J. (1907), "Second catalogue of variable stars", Annals of Harvard College Observatory, 55: 1–94, Bibcode:1907AnHar..55....1C , retrieved 8 January 2025
  13. ↑ Ireland, M. J.; et al. (July 2005), "Dust scattering in the Miras R Car and RR Sco resolved by optical interferometric polarimetry", Monthly Notices of the Royal Astronomical Society, 361 (1): 337–344, arXiv: astro-ph/0505112 , Bibcode:2005MNRAS.361..337I, doi: 10.1111/j.1365-2966.2005.09181.x , S2CID   14724805.
  14. ↑ Mason, B. D.; et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal, 122 (6): 3466, Bibcode:2001AJ....122.3466M, doi: 10.1086/323920 .
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