RV Caeli

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RV Caeli
Caelum constellation map.svg
Red circle.svg
Location of RV Caeli (circled)
Observation data
Epoch J2000       Equinox J2000
Constellation Caelum
Right ascension 04h 28m 09.46368s [1]
Declination −41° 51′ 35.4013″ [1]
Apparent magnitude  (V)6.4±0.01 [2]
Characteristics
Evolutionary stage AGB [3]
Spectral type M1 III [4]
B−V color index +1.64 [5]
Variable type semiregular [6]
Astrometry
Radial velocity (Rv)97.9±0.5 [7]  km/s
Proper motion (μ)RA: −14.75  mas/yr [8]
Dec.: +2.87  mas/yr [8]
Parallax (π)2.4402 ± 0.0229  mas [1]
Distance 1,340 ± 10  ly
(410 ± 4  pc)
Absolute magnitude  (MV)−1.36 [9]
Details
Mass 1.14 [10]   M☉
Radius 107 [11]   R☉
Luminosity 976±30 [12]   L☉
Surface gravity (log g)0.67 [10]   cgs
Temperature 3,843±122 [13]   K
Metallicity [Fe/H]−0.15 [10]   dex
Other designations
4 G. Caeli [14] , CD−42°1510, CPD−42°469, GC  5451, HD  28552, HIP  20856, HR  1429, SAO  216821 [15]
Database references
SIMBAD data

RV Caeli, also known as HD 28552, is a solitary, red hued variable star located in the southern constellation Caelum, the chisel. It has an apparent magnitude of 6.4, [2] placing it near the limit for naked eye visibility. The object is located relatively far at a distance of 1,340 light years based on parallax measurements from Gaia DR3, [1] but is rapidly receding with a heliocentric radial velocity of 98  km/s . [7]

A visual band light curve for RV Caeli, adapted from Tabur et al. (2009). RVCaeLightCurve.png
A visual band light curve for RV Caeli, adapted from Tabur et al. (2009).

Hipparcos has found it to vary between its photometric values of 6.44 and 6.56, [6] which roughly corresponds with the magnitude as seen with the naked eye. It was first suspected of variability in 1970, [17] and a 1982 survey also identified suspected variations. However, it could not confirm it was a variable star. [18] It was confirmed as a variable star in 1999 on the basis of the Hipparcos photometry and given the variable star designation RV Caeli. [19]

RV Caeli is an evolved red giant star with a stellar classification of M1 III. [4] It is currently on the asymptotic giant branch, [3] generating energy via hydrogen and helium shell fusion around an inert carbon core. It has 114% the mass of the Sun [10] but has expanded to over 100 times its girth. [11] It radiates 976 times the luminosity of the Sun [12] from its photosphere at an effective temperature of 3,843  K . [13] RV Caeli is metal deficient, having an iron abundance 70% that of the Sun.

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References

  1. 1 2 3 4 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.
  2. 1 2 Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (March 2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27–L30. Bibcode:2000A&A...355L..27H. ISSN   0004-6361.
  3. 1 2 Eggen, Olin J. (July 1992). "Asymptotic giant branch stars near the sun". The Astronomical Journal. 104: 275. Bibcode:1992AJ....104..275E. doi: 10.1086/116239 . ISSN   0004-6256.
  4. 1 2 Houk, Nancy (1978). Michigan catalogue of two-dimensional spectral types for the HD stars Volume II: Declinations −52° to −41°. Bibcode:1978mcts.book.....H.
  5. ↑ Johnson, H. L.; Mitchell, R. I.; Iriarte, B.; Wisniewski, W. Z. (1966). "UBVRIJKL Photometry of the Bright Stars". Communications of the Lunar and Planetary Laboratory. 4: 99–110. Bibcode:1966CoLPL...4...99J.
  6. 1 2 VSX (25 August 2009). "RV Cae". International Variable Star Index. American Association of Variable Star Observers . Retrieved 30 June 2014.
  7. 1 2 Gontcharov, G. A. (November 2006). "Pulkovo Compilation of Radial Velocities for 35,495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759–771. arXiv: 1606.08053 . Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065. eISSN   1562-6873. ISSN   1063-7737. S2CID   119231169.
  8. 1 2 van Leeuwen, Floor (13 August 2007). "Validation of the new Hipparcos reduction". Astronomy & Astrophysics. 474 (2): 653–664. arXiv: 0708.1752 . Bibcode:2007A&A...474..653V. doi: 10.1051/0004-6361:20078357 . eISSN   1432-0746. ISSN   0004-6361. Hipparcos record for this source at VizieR.
  9. ↑ Anderson, E.; Francis, Ch. (May 2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331–346. arXiv: 1108.4971 . Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. eISSN   1562-6873. ISSN   1063-7737. S2CID   119257644.
  10. 1 2 3 4 Anders, F.; et al. (August 2019). "Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia DR2 stars brighter than G = 18". Astronomy & Astrophysics. 628: A94. arXiv: 1904.11302 . Bibcode:2019A&A...628A..94A. doi: 10.1051/0004-6361/201935765 . eISSN   1432-0746. ISSN   0004-6361.
  11. 1 2 Kervella, Pierre; Arenou, Frédéric; Thévenin, Frédéric (2022). "Stellar and substellar companions from Gaia EDR3". Astronomy & Astrophysics. 657: A7. arXiv: 2109.10912 . Bibcode:2022A&A...657A...7K. doi: 10.1051/0004-6361/202142146 . eISSN   1432-0746. ISSN   0004-6361.
  12. 1 2 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.
  13. 1 2 Stassun, Keivan G.; et al. (9 September 2019). "The Revised TESS Input Catalog and Candidate Target List". The Astronomical Journal. 158 (4): 138. arXiv: 1905.10694 . Bibcode:2019AJ....158..138S. doi: 10.3847/1538-3881/ab3467 . eISSN   1538-3881.
  14. ↑ Gould, Benjamin Apthorp (1878). "Uranometria Argentina : brillantez y posicion de las estrellas fijas, hasta la septima magnitud, comprendidas dentro de cien grados del polo austral : con atlas". Resultados del Observatorio Nacional Argentino. 1. Bibcode:1879RNAO....1.....G.
  15. ↑ "HD 28552". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved September 28, 2022.
  16. ↑ Tabur, V.; Bedding, T. R.; Kiss, L. L.; Moon, T. T.; Szeidl, B.; Kjeldsen, H. (December 2009). "Long-term photometry and periods for 261 nearby pulsating M giants". Monthly Notices of the Royal Astronomical Society. 400 (4): 1945–1961. arXiv: 0908.3228 . Bibcode:2009MNRAS.400.1945T. doi: 10.1111/j.1365-2966.2009.15588.x . S2CID   15358380.
  17. ↑ Eggen, O. J.; Stokes, N. R. (July 1970). "Narrow-Band and Broad-Band Photometry of Red Stars. III. Southern Giants". The Astrophysical Journal. 161: 199. Bibcode:1970ApJ...161..199E. doi: 10.1086/150525 . eISSN   1538-4357. ISSN   0004-637X.
  18. ↑ Rufener, F.; Bartholdi, P. (June 1982). "List of 333 variable, microvariable or suspected variable stars detected in the Geneva photometry". Astronomy and Astrophysics Supplement Series. 48: 503. Bibcode:1982A&AS...48..503R.
  19. ↑ Kazarovets, E. V.; Samus, N. N.; Durlevich, O. V.; Frolov, M. S.; Antipin, S. V.; Kireeva, N. N.; Pastukhova, E. N. (January 1999). "The 74th Special Name-list of Variable Stars". Information Bulletin on Variable Stars. 4659: 1. Bibcode:1999IBVS.4659....1K. ISSN   0374-0676.
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