L2 Puppis

L² Puppis

Observations of L2 Puppis by SPHERE instrument combined with infrared data from NACO on the VLT
Credit: ESO/P. Kervella
Observation data
Epoch J2000      Equinox J2000
Constellation Puppis
Right ascension 07h 13m 32.3187s[1]
Declination −44° 38′ 23.060″[1]
Apparent magnitude (V) 5.10 (SIMBAD)[2]
2.6 - 6 (1971)
6 - 8[3]
Characteristics
Spectral type M5IIIe[2]
U−B color index +1.245[2]
B−V color index +1.63[2]
Astrometry
Radial velocity (Rv)53.0[4] km/s
Proper motion (μ) RA: 107.12[1] mas/yr
Dec.: 325.32[1] mas/yr
Parallax (π)16.46 ± 1.27[1] mas
Distance200 ± 20 ly
(61 ± 5 pc)
Details
Mass1.7[5] M☉
Radius126[5] R☉
Luminosity2,430[5] L☉
Temperature3,380[5] K
Other designations
L2 Puppis, L02 Pup, HR 2748, CD-44 3227, HD 56096, LTT 2769, SAO 218549, HIP 34922.

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 that varies in apparent magnitude from 2.60 down to 6.00 with a period of 140.83 days.[6] The variation in light may be caused by a combination of radial pulsations in the star's atmosphere and by dimming from circumstellar dust.[7] This is most likely an asymptotic giant branch star that has passed through the main sequence and is evolving to become a white dwarf. It is shedding mass at the rate of about 2.2 × 10−9 solar masses per year.[5] Recently the star has had an apparent magnitude range of about 6.9 to 8.[3]

L2 Puppis has a visual 10th magnitude companion about a minute of arc away.[8]

References

  1. 1 2 3 4 5 Perryman, M. A. C.; et al. (July 1997). "The Hipparcos Catalogue". Astronomy & Astrophysics 323: L49–L52. Bibcode:1997A&A...323L..49P.
  2. 1 2 3 4 "V* L02 Pup -- Semi-regular pulsating Star". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2010-10-05.
  3. 1 2 "THE VANNISHING L2 PUPPIS". Sydney City Skywatchers. Retrieved 2012-08-24.
  4. ↑ Wilson, Ralph Elmer (1953). General Catalogue of Stellar Radial Velocities. Washington: Carnegie Institution of Washington. Bibcode:1953QB901.W495.....
  5. 1 2 3 4 5 Winters, J. M.; Le Bertre, T.; Nyman, L.-Å.; Omont, A.; Jeong, K. S. (June 2002). "The hydrodynamical structure of circumstellar envelopes around low mass-loss rate, low outflow velocity AGB stars". Astronomy and Astrophysics 388 (2): 609–614. Bibcode:2002A&A...388..609W. doi:10.1051/0004-6361:20020524.
  6. ↑ Kukarkin, B. V.; Kholopov, P. N.; Pskovsky, Y. P.; Efremov, Y. N.; Kukarkina, N. P.; Kurochkin, N. E.; Medvedeva, G. I. (1971). General Catalogue of Variable Stars, containing information on 20437 variable stars discovered and designated till 1968. (3rd ed.). Bibcode:1971GCVS3.C......0K.
  7. ↑ Bedding, T. R.; Kiss, L. L.; Kjeldsen, H.; Brewer, B. J.; Dind, Z. E.; Kawaler, S. D.; Zijlstra, A. A. (August 2005). "The light curve of the semiregular variable L2 Puppis - II. Evidence for solar-like excitation of the oscillations". Monthly Notices of the Royal Astronomical Society 361 (4): 1375–1381. arXiv:astro-ph/0507471. Bibcode:2005MNRAS.361.1375B. doi:10.1111/j.1365-2966.2005.09281.x.
  8. ↑ James B. (Jim) Kaler. "L2 PUP (L2 Puppis)". University of Illinois. Retrieved 2012-08-24.
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