Pi³ Orionis
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| Observation data Epoch J2000.0 Equinox J2000.0 |
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|---|---|
| Constellation | Orion |
| Right ascension | 04h 49m 50.41091s[1] |
| Declination | +06° 57′ 40.5883″[1] |
| Apparent magnitude (V) | 3.16[2] |
| Characteristics | |
| Spectral type | F6V[2] |
| U−B color index | +0.00[2] |
| B−V color index | +0.46[2] |
| Variable type | Suspected[3] |
| Astrometry | |
| Radial velocity (Rv) | 24.1[4] km/s |
| Proper motion (μ) | RA: 464.06[1] mas/yr Dec.: 11.21[1] mas/yr |
| Parallax (π) | 123.94 ± 0.17[1] mas |
| Distance | 26.32 ± 0.04 ly (8.07 ± 0.01 pc) |
| Absolute magnitude (MV) | 3.65[5] |
| Details | |
| Mass | 1.236[6] M☉ |
| Radius | 1.323 ± 0.004[7] R☉ |
| Luminosity | 2.822 ± 0.030[7] L☉ |
| Surface gravity (log g) | 4.4[8] |
| Temperature | 6,516 ± 19[7] K |
| Metallicity [Fe/H] | 0.02[8] dex |
| Rotational velocity (v sin i) | 17[9] km/s |
| Age | 1.4[5] Gyr |
| Other designations | |
Pi3 Orionis (π3 Ori, π3 Orionis), formally designated Tabit,[11] is a white F-type dwarf star approximately 26 light-years away in the constellation of Orion. It is thought that the star may, in fact, be a binary star system. Though no extrasolar planets have been observed around Pi3 Orionis, the star is considered a prime location for planets as small as the Earth. Pi3 Orionis is the brightest star in the lion's hide (or shield) that Orion is holding.
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[edit] Stellar components
Pi3 Orionis is a dwarf star of spectral type F6 V. Since 1943, the spectrum of this star has served as one of the stable anchor points by which other stars are classified.[12] It has been calculated that the star has 1.2 times the mass of the Sun, 1.3 times the radius, and 3 times the luminosity. It is thought[weasel words] that Pi3 Orionis has a companion star, but the purported companion "B" may not in fact be part of the system.[citation needed]
[edit] Hunt for substellar objects
Although a periodicity of 73.26 days has been observed in the star's radial velocity, it seems likely to be bound more to stellar activity than to a planetary object in close orbit. No substellar companion has been detected so far around Pi3 Orionis and the McDonald Observatory team has set limits to the presence of one or more planets[13] with masses between 0.84 and 46.7 Jupiter masses and average separations spanning between 0.05 and 5.2 astronomical units. Thus, so far it appears that an Earth-like planet could easily orbit the star without any complications.
[edit] See also
[edit] References
- ^ a b c d e van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, Bibcode 2007A&A...474..653V, doi:10.1051/0004-6361:20078357
- ^ a b c d Johnson, H. L.; Morgan, W. W. (1953). "Fundamental stellar photometry for standards of spectral type on the revised system of the Yerkes spectral atlas". Astrophysical Journal 117: 313–352. Bibcode 1953ApJ...117..313J. doi:10.1086/145697.
- ^ Kukarkin, B. V.; et al. (1981). Nachrichtenblatt der Vereinigung der Sternfreunde e.V. (Catalogue of suspected variable stars). Moscow: Academy of Sciences USSR Shternberg. Bibcode 1981NVS...C......0K.
- ^ Evans, D. S. (June 20–24, 1966). "The Revision of the General Catalogue of Radial Velocities". In Batten, Alan Henry; Heard, John Frederick. Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30. University of Toronto: International Astronomical Union. http://adsabs.harvard.edu/abs/1967IAUS...30...57E. Retrieved 2009-09-10.
- ^ a b Holmberg, J.; Nordström, B.; Andersen, J. (July 2009). "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics". Astronomy and Astrophysics, Supplement Series 501 (3): 941−947. Bibcode 2009A&A...501..941H. doi:10.1051/0004-6361/200811191. Note: see VizieR catalogue V/130.
- ^ Takeda, G.; et al. (2007). "Stellar parameters of nearby cool stars. II. Physical properties of ~1000 cool stars from the SPOCS catalog". Astrophysical Journal Supplement Series 168: 297–318. Bibcode 2008yCat..21680297T. Note: see VizieR catalogue J/ApJS/168/297.
- ^ a b c Boyajian, Tabetha S. et al. (February 2012), "Stellar Diameters and Temperatures. I. Main-sequence A, F, and G Stars", The Astrophysical Journal 746 (1): 101, Bibcode 2012ApJ...746..101B, doi:10.1088/0004-637X/746/1/101. See Table 10.
- ^ a b Kuroczkin, D.; Wiszniewski, A. (1997). "The problem of iron abundance in the SMR stars.". Acta Astronomica 27: 145–150. Bibcode 1977AcA....27..145K.
- ^ Bernacca, P. L.; Perinotto, M. (1970). "A catalogue of stellar rotational velocities". Contributi Osservatorio Astronomico di Padova in Asiago 239 (1). Bibcode 1970CoAsi.239....1B.
- ^ "1 Ori -- Variable Star". SIMBAD. Centre de Données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=1+Ori. Retrieved 2011-01-07.
- ^ http://www.astro.wisc.edu/~dolan/constellations/hr/1543.html
- ^ Garrison, R. F. (December 1993), "Anchor Points for the MK System of Spectral Classification", Bulletin of the American Astronomical Society 25: 1319, Bibcode 1993AAS...183.1710G, http://www.astro.utoronto.ca/~garrison/mkstds.html, retrieved 2012-02-04
- ^ Wittenmyer, Robert A.; et al. (July 2006). "Detection Limits from the McDonald Observatory Planet Search Program". The Astronomical Journal 132 (1): 177–188. arXiv:astro-ph/0604171. Bibcode 2006AJ....132..177W. doi:10.1086/504942.
[edit] External links
- "Pi3 Orionis 2?". SolStation. http://www.solstation.com/stars/pi3ori2.htm. Retrieved 2008-07-11.
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