Astronomy:Pi1 Orionis
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| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Orion |
| Right ascension | 04h 54m 53.72877s[1] |
| Declination | +10° 09′ 02.9952″[1] |
| Apparent magnitude (V) | 4.74[2] |
| Characteristics | |
| Spectral type | A3 Va[3] |
| U−B color index | +0.09[2] |
| B−V color index | +0.08[2] |
| Astrometry | |
| Proper motion (μ) | RA: +41.49[1] mas/yr Dec.: −128.73[1] mas/yr |
| Parallax (π) | 28.04 ± 0.25[1] mas |
| Distance | 116 ± 1 ly (35.7 ± 0.3 pc) |
| Absolute magnitude (MV) | 1.71±0.09[4] |
| Details[4] | |
| Mass | 1.90+0.08 −0.09 M☉ |
| Radius | 1.73±0.13 R☉ |
| Luminosity | 16.91+1.42 −1.29 L☉ |
| Surface gravity (log g) | 4.22+0.04 −0.05 cgs |
| Temperature | 8,900±131 K |
| Metallicity [Fe/H] | −0.12+0.14 −0.16 dex |
| Rotational velocity (v sin i) | 120[5] km/s |
| Age | 100[6] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Pi1 Orionis (π1 Ori, π1 Orionis) is a star in the equatorial constellation of Orion. It is faintly visible to the naked eye with an apparent visual magnitude of 4.74.[2] Based upon an annual parallax shift of 28.04 mas,[1] it is located about 116 light-years from the Sun.
This is an A-type main-sequence star with a stellar classification of A3 Va.[3] It is a Lambda Boötis star,[8] which means the spectrum shows lower-than-expected abundances for heavier elements.[9] Pi1 Orionis is a relatively young star, just 100 million years old,[6] and is spinning fairly rapidly with a projected rotational velocity of 120 km/s.[5] It has nearly double the mass of the Sun and 173% of the Sun's radius. The star radiates 16.9 times the solar luminosity from its outer atmosphere at an effective temperature of 8,900 K.[4]
An infrared excess indicates there is a debris disk with a temperature of 80 K orbiting 49 astronomical unit|AU from the star. The dust has a combined mass 2.2% that of the Earth.[6]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V.
- ↑ 2.0 2.1 2.2 2.3 Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data (SIMBAD), Bibcode: 1986EgUBV........0M.
- ↑ 3.0 3.1 Gray, R. O. et al. (July 2006), "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample", The Astronomical Journal 132 (1): 161–170, doi:10.1086/504637, Bibcode: 2006AJ....132..161G.
- ↑ 4.0 4.1 4.2 Murphy, S. J.; Paunzen, E.; Bedding, T. R.; Walczak, P.; Huber, D. (2020-06-01). "The pulsation properties of λ bootis stars I. the southern TESS sample". Monthly Notices of the Royal Astronomical Society 495 (2): 1888–1912. doi:10.1093/mnras/staa1271. ISSN 0035-8711. Bibcode: 2020MNRAS.495.1888M.
- ↑ 5.0 5.1 Royer, F. et al. (February 2007), "Rotational velocities of A-type stars. III. Velocity distributions", Astronomy and Astrophysics 463 (2): 671–682, doi:10.1051/0004-6361:20065224, Bibcode: 2007A&A...463..671R.
- ↑ 6.0 6.1 6.2 Rhee, Joseph H. et al. (May 2007), "Characterization of Dusty Debris Disks: The IRAS and Hipparcos Catalogs", The Astrophysical Journal 660 (2): 1556–1571, doi:10.1086/509912, Bibcode: 2007ApJ...660.1556R.
- ↑ "* pi.01 Ori". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=%2A+pi.01+Ori.
- ↑ Gray, R. O.; Corbally, C. J. (August 1993), "A search for Lambda Bootis stars in OB associations", Astronomical Journal 106 (2): 632–636, doi:10.1086/116668, Bibcode: 1993AJ....106..632G.
- ↑ Kamp, I. et al. (April 2008), "λ Bootis stars: Current status and new insights from Spitzer", Contributions of the Astronomical Observatory Skalnaté Pleso 38 (2): 147–156, Bibcode: 2008CoSka..38..147K.
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