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Pi5 Orionis

From Wikipedia, the free encyclopedia

For other stars with this Bayer designation, see Pi Orionis.
π5 Orionis
Location of π5 Orionis (circled)
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Orion
Right ascension 04h 54m 15.09604s[1]
Declination +02° 26′ 26.4231″[1]
Apparent magnitude (V) 3.69[2]
Characteristics
Spectral type B2 III[3]
U−B color index −0.81[2]
B−V color index −0.18[2]
Variable type Ellipsoidal[4] (SPB?)[5]
Astrometry
Radial velocity (Rv)+23.4[6] km/s
Proper motion (μ) RA: +0.55[1] mas/yr
Dec.: +0.61[1] mas/yr
Parallax (π)2.43 ± 0.39 mas[1]
Distanceapprox. 1,300 ly
(approx. 410 pc)
Absolute magnitude (MV)−4.3[7]
Orbit[5]
Period (P)3.700373 d
Semi-major axis (a)25.9 AU
Eccentricity (e)0.083±0.040
Inclination (i)34°
Periastron epoch (T)2,433,341.088±0.010 JD
Semi-amplitude (K1)
(primary)		60.41±1.99 km/s
Details
π5 Ori A
Mass12[5] M☉
Radius12[5] R☉
Luminosity11,262[8] L☉
Surface gravity (log g)3.51[9] cgs
Temperature14,496[8] K
Metallicity [Fe/H]−0.28[9] dex
Rotational velocity (v sin i)90[10] km/s
Age15.8±0.2[11] Myr
π5 Ori B
Mass5.0[5] M☉
Radius2.8 - 3.8[5] R☉
Luminosity525 - 741[5] L☉
Surface gravity (log g)3.98 - 4.24[5] cgs
Temperature15,596 - 16,520[5] K
Other designations
π5 Ori, 8 Orionis, BD+02°810, HD 31237, HIP 22797, HR 1567, SAO 112197[12]
Database references
SIMBADdata

Pi5 Orionis (π5 Ori, π5 Orionis) is a binary star system in the constellation Orion. It has an apparent visual magnitude of 3.69,[2] which is bright enough to be visible to the naked eye on a clear night. Based upon an annual parallax shift of 2.43 mas,[1] it is around 1,300 light-years distant from the Sun.

A light curve for Pi5 Oronis, plotted from TESS data[13]

This is a single-lined[3] spectroscopic binary star system in a circular orbit with an orbital period of 3.7005 days.[14] It is an ellipsoidal variable, which means the orbit is sufficiently close that the shapes of the components are being distorted by their mutual gravitation. This is causing the visual magnitude of the system to vary regularly by 0m.05 over the course of each orbit, as the orientation of the stars change with respect to the Earth.[4] Detailed analysis of the light curve suggests that the primary star is also pulsating and is probably a Slowly pulsating B-type star.[5]

The primary component is a B-type giant star with a stellar classification of B2 III.[3] It is only about 16 million years old[11] and spins with a projected rotational velocity of 90 km/s.[10] Despite the spectral class, the primary star is thought to be at or near the end of its main sequence evolution.[5] It has about 12.5 times the mass of the Sun and radiates 11,262[8] times the solar luminosity from its outer atmosphere at an effective temperature of 14,496 K.[8]

The secondary star is not detectable clearly, but modelling of the brightness variations and orbit suggest that it is a main sequence star with a spectral class of about B6. It is smaller, cooler, and much less luminous than the primary, and orbits at about 26 astronomical units.[5]

References

  1. ^ a b c d e f 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.
  2. ^ a b c d Crawford, D. L.; et al. (1971), "Four-color, H-beta, and UBV photometry for bright B-type stars in the northern hemisphere", The Astronomical Journal, 76: 1058, Bibcode:1971AJ.....76.1058C, doi:10.1086/111220.
  3. ^ a b c Chini, R.; et al. (2012), "A spectroscopic survey on the multiplicity of high-mass stars", Monthly Notices of the Royal Astronomical Society, 424 (3): 1925, arXiv:1205.5238, Bibcode:2012MNRAS.424.1925C, doi:10.1111/j.1365-2966.2012.21317.x, S2CID 119120749.
  4. ^ a b Morris, S. L. (August 1985), "The ellipsoidal variable stars", Astrophysical Journal, Part 1, 295: 143–152, Bibcode:1985ApJ...295..143M, doi:10.1086/163359.
  5. ^ a b c d e f g h i j k l Jerzykiewicz, M.; Pigulski, A.; Handler, G.; Moffat, A. F. J.; Popowicz, A.; Wade, G. A.; Zwintz, K.; Pablo, H. (2020). "BRITE-Constellation photometry of π5 Orionis, an ellipsoidal SPB variable". Monthly Notices of the Royal Astronomical Society. 496 (2): 2391. arXiv:2006.05178. Bibcode:2020MNRAS.496.2391J. doi:10.1093/mnras/staa1665.
  6. ^ Evans, D. S. (June 20–24, 1966), "The Revision of the General Catalogue of Radial Velocities", in Batten, Alan Henry; Heard, John Frederick (eds.), Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30, vol. 30, University of Toronto: International Astronomical Union, p. 57, Bibcode:1967IAUS...30...57E.
  7. ^ Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID 119257644.
  8. ^ a b c d McDonald, I.; et al. (2012), "Fundamental Parameters and Infrared Excesses of Hipparcos Stars", Monthly Notices of the Royal Astronomical Society, 427 (1): 343–57, arXiv:1208.2037, Bibcode:2012MNRAS.427..343M, doi:10.1111/j.1365-2966.2012.21873.x, S2CID 118665352.
  9. ^ a b Soubiran, C.; et al. (June 2010), "The PASTEL catalogue of stellar parameters", Astronomy and Astrophysics, 515: A111, arXiv:1004.1069, Bibcode:2010A&A...515A.111S, doi:10.1051/0004-6361/201014247, S2CID 118362423.
  10. ^ a b Abt, Helmut A.; Boonyarak, Chayan (November 2004), "Tidal Effects in Binaries of Various Periods", The Astrophysical Journal, 616 (1): 562–566, Bibcode:2004ApJ...616..562A, doi:10.1086/423795.
  11. ^ a b Tetzlaff, N.; et al. (January 2011), "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun", Monthly Notices of the Royal Astronomical Society, 410 (1): 190–200, arXiv:1007.4883, Bibcode:2011MNRAS.410..190T, doi:10.1111/j.1365-2966.2010.17434.x, S2CID 118629873.
  12. ^ "pi.05 Ori". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2016-11-18.{{cite web}}: CS1 maint: postscript (link)
  13. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 9 December 2022.
  14. ^ Pourbaix, D.; et al. (2004), "SB9: The ninth catalogue of spectroscopic binary orbits", Astronomy & Astrophysics, 424 (2): 727–732, arXiv:astro-ph/0406573, Bibcode:2004A&A...424..727P, doi:10.1051/0004-6361:20041213, S2CID 119387088.

External links

  • Kaler, James B. (February 6, 2009), "Pi-5 Orionis", Stars, University of Illinois, retrieved 2016-11-22.
This page was last edited on 11 December 2022, at 17:42
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