R Leporis (R Lep), sometimes called Hind's Crimson Star,[7] is a well-known variable star in the constellation Lepus, near its border with Eridanus. It is designated "R" in the chart to the right.[1]
It is a carbon star which appears distinctly red. It is named after famous British astronomer J. R. Hind, who observed it in 1845. Its apparent 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] R Leporis is too far from earth for its parallax to be measured effectively; 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] It was estimated to be around 1,350 light-years distant in a 2012 paper, shining with a luminosity approximately 6,689 times that of the Sun and has a surface temperature of 2,980 K.[9]
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 its visible light spectrum. The star's discoverer, Hind, reported that it appeared "like a drop of blood on a black field."[7]
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.
^ abcdefghV* R Lep -- Variable Star of Mira Cet type, database entry, SIMBAD. Accessed on line November 19, 2009.
^ abcR Lep, database entry, The combined table of GCVS Vols I-III and NL 67-78 with improved coordinates, General Catalogue of Variable Stars 2017-06-20 at the Wayback Machine, Sternberg Astronomical Institute, Moscow, Russia. Accessed on line November 19, 2009.
^ abcHR 1607, database entry, The Bright Star Catalogue, 5th Revised Ed. (Preliminary Version), D. Hoffleit and W. H. Warren, Jr., CDS ID V/50. Accessed on line November 19, 2009.
^ abMcDonald, I.; De Beck, E.; Zijlstra, A. A.; Lagadec, E. (2018). "Pulsation-triggered dust production by asymptotic giant branch stars". Monthly Notices of the Royal Astronomical Society. 481 (4): 4984. arXiv:1809.07965. Bibcode:2018MNRAS.481.4984M. doi:10.1093/mnras/sty2607. S2CID 118969263.
^Hofmann, K.-H.; Eberhardt, M.; Driebe, T.; Schertl, D.; Scholz, M.; Schoeller, M.; Weigelt, G.; Wittkowski, M.; Woodruff, H. C. (2005). "Interferometric observations of the Mira star o Ceti with the VLTI/VINCI instrument in the near-infrared". Proceedings of the 13th Cambridge Workshop on Cool Stars. 560: 651. Bibcode:2005ESASP.560..651H.
^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.
^ abRichard Hinckley Allen (1899). Star-names and Their Meanings. New York: G.E. Stechert. p. 269.
^Guandalini, 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.
^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): 343–57. arXiv:1208.2037. Bibcode:2012MNRAS.427..343M. doi:10.1111/j.1365-2966.2012.21873.x. S2CID 118665352.
^"ALMA achieves its highest resolution observations". www.eso.org. Retrieved 15 November 2023.
^"Download Data". aavso.org. AAVSO. Retrieved 1 October 2021.
External linksedit
Best of the Advanced Observation Program: R Leporis 2015-05-24 at the Wayback Machine
USA Today.com - NightSky: The Hare and the Dove
Smoky Mountain Astronomical Society - Hind's Crimson Star: R Leporis 2016-03-03 at the Wayback Machine
Geody Hinds Crimson Star
Observations of R LEP from AAVSO
Astronomy picture of the day
April 13, 2024
leporis, sometimes, called, hind, crimson, star, well, known, variable, star, constellation, lepus, near, border, with, eridanus, designated, chart, right, location, constellation, lepus, observation, dataepoch, j2000, equinox, j2000, icrs, constellation, lepu. R Leporis R Lep sometimes called Hind s Crimson Star 7 is a well known variable star in the constellation Lepus near its border with Eridanus It is designated R in the chart to the right 1 R LeporisLocation of R Leporis in the constellation Lepus Observation dataEpoch J2000 0 Equinox J2000 0 ICRS Constellation LepusRight ascension 04h 59m 36 3487s 1 Declination 14 48 22 518 1 Apparent magnitude V 5 5 to 11 7 2 CharacteristicsSpectral type C7 6e N6e 2 B V color index 5 74 3 R I color index 1 47 3 Variable type Mira 2 AstrometryRadial velocity Rv 32 4 2 1 km sProper motion m RA 7 51 1 mas yr Dec 4 27 1 mas yrParallax p 2 42 1 02 mas 1 Distance418 4 pcDetailsRadius400 90 5 R Luminosity5 149 4 L Temperature2 290 6 KOther designationsR Lep AAVSO 0455 14 BD 15 915 GC 6093 HD 31996 HIP 23203 HR 1607 IRC 10080 PPM 215123 RAFGL 667 SAO 150058 1 Database referencesSIMBADdataIt is a carbon star which appears distinctly red It is named after famous British astronomer J R Hind who observed it in 1845 Its apparent 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 R Leporis is too far from earth for its parallax to be measured effectively 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 It was estimated to be around 1 350 light years distant in a 2012 paper shining with a luminosity approximately 6 689 times that of the Sun and has a surface temperature of 2 980 K 9 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 its visible light spectrum The star s discoverer Hind reported that it appeared like a drop of blood on a black field 7 R Leporis as imaged by ALMA 10 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 11 References edit a b c d e f g h V R Lep Variable Star of Mira Cet type database entry SIMBAD Accessed on line November 19 2009 a b c R Lep database entry The combined table of GCVS Vols I III and NL 67 78 with improved coordinates General Catalogue of Variable Stars Archived 2017 06 20 at the Wayback Machine Sternberg Astronomical Institute Moscow Russia Accessed on line November 19 2009 a b c HR 1607 database entry The Bright Star Catalogue 5th Revised Ed Preliminary Version D Hoffleit and W H Warren Jr CDS ID V 50 Accessed on line November 19 2009 a b McDonald I De Beck E Zijlstra A A Lagadec E 2018 Pulsation triggered dust production by asymptotic giant branch stars Monthly Notices of the Royal Astronomical Society 481 4 4984 arXiv 1809 07965 Bibcode 2018MNRAS 481 4984M doi 10 1093 mnras sty2607 S2CID 118969263 Hofmann K H Eberhardt M Driebe T Schertl D Scholz M Schoeller M Weigelt G Wittkowski M Woodruff H C 2005 Interferometric observations of the Mira star o Ceti with the VLTI VINCI instrument in the near infrared Proceedings of the 13th Cambridge Workshop on Cool Stars 560 651 Bibcode 2005ESASP 560 651H Lombaert R Decin L Royer P De Koter A Cox N L J Gonzalez Alfonso E Neufeld D De Ridder J Agundez 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 amp Astrophysics 588 A124 arXiv 1601 07017 Bibcode 2016A amp A 588A 124L doi 10 1051 0004 6361 201527049 S2CID 62787287 a b Richard Hinckley Allen 1899 Star names and Their Meanings New York G E Stechert p 269 Guandalini R Cristallo S 2013 Luminosities of carbon rich asymptotic giant branch stars in the Milky Way Astronomy amp Astrophysics 555 7 arXiv 1305 4203 Bibcode 2013A amp A 555A 120G doi 10 1051 0004 6361 201321225 S2CID 54918450 A120 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 57 arXiv 1208 2037 Bibcode 2012MNRAS 427 343M doi 10 1111 j 1365 2966 2012 21873 x S2CID 118665352 ALMA achieves its highest resolution observations www eso org Retrieved 15 November 2023 Download Data aavso org AAVSO Retrieved 1 October 2021 External links editBest of the Advanced Observation Program R Leporis Archived 2015 05 24 at the Wayback Machine USA Today com NightSky The Hare and the Dove Smoky Mountain Astronomical Society Hind s Crimson Star R Leporis Archived 2016 03 03 at the Wayback Machine Geody Hinds Crimson Star Observations of R LEP from AAVSO Astronomy picture of the day Retrieved from https en wikipedia org w index php title R Leporis amp oldid 1218505112, wikipedia, wiki, book, books, library,
