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R Leporis

From Wikipedia, the free encyclopedia
Star in the constellation Lepus
R Leporis

Location of R Leporis in the constellation Lepus.
Observation data
EpochJ2000.0      EquinoxJ2000.0 (ICRS)
ConstellationLepus
Right ascension04h 59m 36.3487s[1]
Declination−14° 48′ 22.518″[1]
Apparent magnitude (V)5.5 to 11.7[2]
Characteristics
Spectral typeC7,6e(N6e)[2]
B−Vcolor index+5.74[3]
R−Icolor index+1.47[3]
Variable typeMira[2]
Astrometry
Radial velocity (Rv)32.4 ± 2[1] km/s
Proper motion (μ)RA: 6.798mas/yr[4]
Dec.: −1.263mas/yr[4]
Parallax (π)2.1914±0.0602 mas[4]
Distance1,490 ± 40 ly
(460 ± 10 pc)
Details
Mass1.00[5] – 2.02[6] M☉
Radius710 – 910[7][a] R☉
Luminosity13,200[8] L☉
Surface gravity (log g)−0.6[6] cgs
Temperature2,290[9] K
Metallicity [Fe/H]−0.409[6] dex
Other designations
R Lep,AAVSO 0455-14,BD−15 915,GC 6093,HD 31996,HIP 23203,HR 1607,SAO 150058,PPM 215123[1]
Database references
SIMBADdata

R Leporis (R Lep), sometimes calledHind's Crimson Star,[10] is a well-knownvariable star in the constellationLepus, near its border withEridanus.

It is acarbon star which appears distinctly red. It is named after famous British astronomerJ. R. Hind, who observed it in 1845. Itsapparent magnitude varies from +5.5 to +11.7 with a period of 418–441 days; recent measurements give a period of 427.07 days. There may be a secondary period of 40 years.[3] Guandalini and Cristallo calculated the luminosity of Mira variables based on their periods. Using a period of 427.07 days, they calculated the bolometric luminosity to be 13,200 L☉.[8]

R Leporis has often been reported as an intense smoky red color, although this is not pronounced when the star is near its maximum brightness. It is reddest when it is dimmest, which occurs every 14.5 months. During these periods it is a candidate for the most-visible reddest star, but this claim is questionable. The red coloration may be caused by carbon in the star's outer atmosphere filtering out the blue part of itsvisible light spectrum. The star's discoverer, Hind, reported that it appeared "like a drop of blood on a black field."[10]

  • R Leporis as imaged by ALMA[11]
    R Leporis as imaged by ALMA[11]
  • An image of the carbon star R Leporis as seen in binoculars. R Leporis is the red star right of centre. The bright star in the lower left corner is Mu Leporis.
    An image of the carbon star R Leporis as seen in binoculars. R Leporis is the red star right of centre. The bright star in the lower left corner is Mu Leporis.
  • The light curve of R Leporis from AAVSO V band data[12]
    Thelight curve of R Leporis from AAVSOV band data[12]

Notes

[edit]
  1. ^Calculated via the equation R = 0.1075 • 𝜃 • d, where R is the radius (in solar radii/R☉), 𝜃 is the angular diameter inarcseconds andd is the distance inparsecs. Angular diameters of 14 to 18 milliarcseconds (0.014-0.018 arcseconds) and a distance of 471parsecs were adopted.

References

[edit]
  1. ^abcd"R Leporis".SIMBAD.Centre de données astronomiques de Strasbourg. RetrievedNovember 19, 2009.
  2. ^abcR Lep, database entry,The combined table of GCVS Vols I-III and NL 67-78 with improved coordinates, General Catalogue of Variable StarsArchived 2017-06-20 at theWayback Machine, Sternberg Astronomical Institute, Moscow, Russia. Accessed on line November 19, 2009.
  3. ^abcHR 1607, database entry, The Bright Star Catalogue, 5th Revised Ed. (Preliminary Version), D. Hoffleit and W. H. Warren, Jr.,CDS IDV/50. Accessed on line November 19, 2009.
  4. ^abVallenari, 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 atVizieR.
  5. ^Rau, G.; Hron, J.; Paladini, C.; Aringer, B.; Eriksson, K.; Marigo, P.; Nowotny, W.; Grellmann, R. (2017-04-01). "The adventure of carbon stars. Observations and modeling of a set of C-rich AGB stars".Astronomy and Astrophysics.600: A92.arXiv:1701.04331.Bibcode:2017A&A...600A..92R.doi:10.1051/0004-6361/201629337.ISSN 0004-6361.
  6. ^abcAnders, F.; Khalatyan, A.; Queiroz, A. B. A.; Chiappini, C.; Ardèvol, J.; Casamiquela, L.; Figueras, F.; Jiménez-Arranz, Ó.; Jordi, C.; Monguió, M.; Romero-Gómez, M.; Altamirano, D.; Antoja, T.; Assaad, R.; Cantat-Gaudin, T. (2022-02-01). "Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia EDR3 stars brighter than G = 18.5".Astronomy and Astrophysics.658: A91.arXiv:2111.01860.Bibcode:2022A&A...658A..91A.doi:10.1051/0004-6361/202142369.ISSN 0004-6361.Database atVizieR.
  7. ^Asaki, Yoshiharu; Maud, Luke T.; Francke, Harold; Nagai, Hiroshi; Petry, Dirk; Fomalont, Edward B.; Humphreys, Elizabeth; Richards, Anita M. S.; Wong, Ka Tat; Dent, William; Hirota, Akihiko; Fernandez, Jose Miguel; Takahashi, Satoko; Hales, Antonio S. (November 2023)."ALMA High-frequency Long Baseline Campaign in 2021: Highest Angular Resolution Submillimeter Wave Images for the Carbon-rich Star R Lep".The Astrophysical Journal.958 (1): 86.arXiv:2310.09664.Bibcode:2023ApJ...958...86A.doi:10.3847/1538-4357/acf619.ISSN 0004-637X.
  8. ^abGuandalini, R.; Cristallo, S. (2013). "Luminosities of carbon-rich asymptotic giant branch stars in the Milky Way".Astronomy & Astrophysics.555: 7.arXiv:1305.4203.Bibcode:2013A&A...555A.120G.doi:10.1051/0004-6361/201321225.S2CID 54918450. A120.
  9. ^Lombaert, R.; Decin, L.; Royer, P.; De Koter, A.; Cox, N. L. J.; González-Alfonso, E.; Neufeld, D.; De Ridder, J.; Agúndez, M.; Blommaert, J. A. D. L.; Khouri, T.; Groenewegen, M. A. T.; Kerschbaum, F.; Cernicharo, J.; Vandenbussche, B.; Waelkens, C. (2016). "Constraints on the H2O formation mechanism in the wind of carbon-rich AGB stars".Astronomy & Astrophysics.588: A124.arXiv:1601.07017.Bibcode:2016A&A...588A.124L.doi:10.1051/0004-6361/201527049.S2CID 62787287.
  10. ^abRichard Hinckley Allen (1899).Star-names and Their Meanings. New York: G.E. Stechert. p. 269.
  11. ^"ALMA achieves its highest resolution observations".www.eso.org. Retrieved15 November 2023.
  12. ^"Download Data".aavso.org. AAVSO. Retrieved1 October 2021.

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