T Leporis

In today's world, T Leporis is a topic that has sparked a lot of interest and debate. From its origins to its evolution today, T Leporis has had a significant impact on various areas of society. Its influence has extended to aspects such as economics, politics, culture and technology, generating both admiration and controversy. In this article, we will explore in depth the various aspects related to T Leporis, analyzing its impact in different contexts and examining the implications it has today.

T Leporis

T Leporis (below) compared to the Sun and Earth's orbit (above)
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Lepus
Right ascension 05h 04m 50.85s[1]
Declination −21° 54′ 16.5″[1]
Apparent magnitude (V) 7.4 - 14.3[2]
Characteristics
Spectral type M6e-M9e[2]
Variable type Mira[2]
Astrometry
Radial velocity (Rv)−4[3] km/s
Proper motion (μ) RA: +13.59 mas/yr[4]
Dec.: −34.55 mas/yr[4]
Parallax (π)3.06±0.04 mas[4]
Distance1,066±13 ly
(327±4 pc)[4]
Details
Mass2.7[5] M☉
Radius204[4] R☉
Surface gravity (log g)−0.5[5] cgs
Temperature2,800[5] K
Other designations
T Lep, BD−22°995, CD−22°995, HD 32803, HIP 23636
Database references
SIMBADdata

T Leporis (T Lep / HD 32803 / HIP 23636) is a variable star in the constellation of Lepus, the Hare. It is located half a degree from ε Leporis in the sky; its distance is approximately 1,100 light years from the Solar System. It has the spectral type M6ev, and is a Mira variable — as is R Leporis, in the same constellation — whose apparent magnitude varies between +7.40 and +14.30 with a period of 368.13 days.[2]

The annual parallax of T Leporis was measured by the Hipparcos mission, but the results were hopelessly imprecise.[6] The parallax from Gaia Data Release 2 is more accurate and yields a distance of 340±20 pc.[1] The distance has also been measured using very-long-baseline interferometry and found to be 327±4 pc.[4]

The visual band light curve of T Leporis, from AAVSO data[7]

Mira variables are some of the major sources of molecules and dust in the Universe. With each pulsation, T Leporis expels matter into space, each year losing an amount equivalent to the mass of Earth. Images of T Leporis obtained with the Very Large Telescope interferometer of the European Southern Observatory (ESO) have revealed a shell of gas and dust surrounding the star, whose diameter is some 100 times larger than that of the Sun.[8] Given the great distance at which this class of stars lie, its apparent angular diameter — despite its enormous size — is no more than a millionth of the solar apparent angular diameter.

See also

References

  1. ^ a b c 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.
  2. ^ a b c d Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1: B/gcvs. Bibcode:2009yCat....102025S.
  3. ^ Gontcharov, G. A. (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. S2CID 119231169.
  4. ^ a b c d e Nakagawa, Akiharu; Omodaka, Toshihiro; Handa, Toshihiro; Honma, Mareki; Kawaguchi, Noriyuki; Kobayashi, Hideyuki; Oyama, Tomoaki; Sato, Katsuhisa; Shibata, Katsunori M.; Shizugami, Makoto; Tamura, Yoshiaki; Ueno, Yuji (2014). "VLBI astrometry of AGB variables with VERA: A Mira-type variable T Lepus". Publications of the Astronomical Society of Japan. 66 (6): 101. arXiv:1404.4463. Bibcode:2014PASJ...66..101N. doi:10.1093/pasj/psu103. S2CID 118635632.
  5. ^ a b c Pérez-Mesa, V.; Zamora, O.; García-Hernández, D. A.; Plez, B.; Manchado, A.; Karakas, A. I.; Lugaro, M. (2017). "Rubidium and zirconium abundances in massive Galactic asymptotic giant branch stars revisited". Astronomy and Astrophysics. 606: A20. arXiv:1706.02268. Bibcode:2017A&A...606A..20P. doi:10.1051/0004-6361/201731245. S2CID 55190629.
  6. ^ Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID 18759600.
  7. ^ "Download Data". aavso.org. AAVSO. Retrieved 1 October 2021.
  8. ^ "Unique Details Of Double Star In Orion Nebula And Star T Leporis Captured By 'Virtual' Telescope". ScienceDaily. 19 February 2009.