R Leonis

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R Leonis
Leo constellation map.svg
Red circle.svg
Location of R Leonis (circled)
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Leo
Right ascension 09h 47m 33.4904s
Declination +11° 25′ 43.646″
Apparent magnitude (V) 4.4 - 11.3[1]
Characteristics
Spectral type M8IIIe[2]
Apparent magnitude (J) -0.7[3]
B−V color index 1.26
Variable type Mira-type
Astrometry
Distance 267-370 ly
(82[2]-113.5[4] pc)
Details
Mass 0.7[4] M
Radius 299[2], 320-350[5] R
Luminosity 5,617[2]-8,090[5] L
Temperature 2,890[2], 2,930-3,080[5] K
Other designations
R Leo, HIP 48036, HD 84748, HR 3882, BD+12° 2096, SAO 98769
Database references
SIMBAD data

R Leonis is a red giant Mira-type variable star located approximately 300 light years away in the constellation Leo.

The apparent magnitude of R Leonis varies between 4.31 and 11.65 with a period of 312 days. At maximum it can be seen with the naked eye, while at minimum a telescope of at least 7 cm is needed. The star's effective temperature is estimated 2,890 kelvins and radius spans 299 solar radii (208,000,000 kilometres; 1.39 astronomical units)[2], roughly Mars's orbital zone.

Possible planet[edit]

Artistic rendering of R Leonis's putative evaporating planetary companion

In 2009 Wiesemeyer et al.[4] proposed that quasi-periodic fluctuations observed for the star R Leonis may be due to the presence of an evaporating substellar companion, probably an extrasolar planet. They have inferred a putative mass for the orbiting body of twice the mass of Jupiter, orbital period of 5.2 years and likely orbital separation of 2.7 astronomical units. If confirmed such a planetary object could likely be an evaporating planet, with long comet-like trail as hinted by intense SiO maser emissions.

The R Leonis planetary system
Companion
(in order from star)
Mass Semimajor axis
(AU)
Orbital period
(days)
Eccentricity Inclination Radius
b (unconfirmed) ≥2 MJ ≥2.7 1898 0

References[edit]

  1. ^ "GCVS Query=R Leo". General Catalogue of Variable Stars @ Sternberg Astronomical Institute, Moscow, Russia. Retrieved 2012-08-22. 
  2. ^ a b c d e f De Beck, E.; Decin, L.; De Koter, A.; Justtanont, K.; Verhoelst, T.; Kemper, F.; Menten, K. M. (2010). "Probing the mass-loss history of AGB and red supergiant stars from CO rotational line profiles. II. CO line survey of evolved stars: Derivation of mass-loss rate formulae". Astronomy and Astrophysics. 523: A18. arXiv:1008.1083Freely accessible. Bibcode:2010A&A...523A..18D. doi:10.1051/0004-6361/200913771. 
  3. ^ "V* R Leo". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2012-08-21. 
  4. ^ a b c Wiesemeyer; et al. (2009). "Precessing planetary magnetospheres in SiO stars?. First detection of quasi-periodic polarization fluctuations in R Leonis and V Camelopardalis". Astronomy and Astrophysics. 498 (3): 801–810. arXiv:0809.0359Freely accessible. Bibcode:2009A&A...498..801W. doi:10.1051/0004-6361/200811242. 
  5. ^ a b c Fedele; et al. (2005). "The K -Band Intensity Profile of R Leonis Probed by VLTI/VINCI". Astronomy and Astrophysics. 431 (3): 1019–1026. arXiv:astro-ph/0411133Freely accessible. Bibcode:2005A&A...431.1019F. doi:10.1051/0004-6361:20042013. 

External links[edit]