Psi Crateris

Psi Crateris
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Crater
Right ascension 11h 12m 30.37188s[1]
Declination −18° 29′ 59.4995″[1]
Apparent magnitude (V) 6.13[2] (6.24 + 8.34)[3]
Characteristics
Spectral type A0 V[4] (A0 + A3)[5]
B−V color index −0.01[2]
Astrometry
Radial velocity (Rv)+14.2±0.7[6] km/s
Proper motion (μ) RA: −20.48[1] mas/yr
Dec.: −24.80[1] mas/yr
Parallax (π)6.50 ± 0.71[1] mas
Distanceapprox. 500 ly
(approx. 150 pc)
Absolute magnitude (MV)+0.21[7]
Orbit[8]
Period (P)365.68±8.02 yr
Semi-major axis (a)0.553±0.022″
Eccentricity (e)0.434±0.014
Inclination (i)99.8±0.8°
Longitude of the node (Ω)325.3±0.6°
Periastron epoch (T)1983.92 ± 3.59
Argument of periastron (ω)
(secondary)		337.3±6.7°
Details
ψ Crt A
Luminosity75[9] L☉
Surface gravity (log g)3.8[10] cgs
Temperature9,199[9] K
Metallicity [Fe/H]0.0[10] dex
Rotational velocity (v sin i)33[4] km/s
Other designations
ψ Crt, BD−17° 3321, HD 97411, HIP 54742, HR 4347, SAO 156528, WDS J11125-1830AB.[11]
Database references
SIMBADψ Crt
ψ Crt A
ψ Crt B

Psi Crateris, Latinized from ψ Crateris, is the Bayer designation for a visual binary[8] star system in the southern constellation of Crater. It is faintly visible to the naked eye with an apparent visual magnitude of 6.13.[2] According to the Bortle scale, it requires dark suburban or rural skies to view. Based upon an annual parallax shift of 6.5 mas,[1] the system is located approximately 500 light years away from the Sun.

The components in this star system have an orbital period of about 366 years with an eccentricity of 0.43.[8] The angular size of the orbit's semimajor axis is about half an arc second. The primary member, component A, is an ordinary A-type main sequence star with a visual magnitude of 6.24 and a stellar classification of A0 V.[4] It was a candidate λ Boötis star, but this was later rejected when the spectrum was found to be normal. Any peculiarities may have instead resulted from the overlapping spectra of the two stars.[12] The star is radiating about 75 times the solar luminosity from it outer atmosphere at an effective temperature of 9,199 K.[9] The fainter secondary, component B, has a visual magnitude of 8.34[3] and a class of A3.[5]

References

  1. 1 2 3 4 5 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.
  2. 1 2 3 Nicolet, B. (1978), "Photoelectric photometric Catalogue of homogeneous measurements in the UBV System", Astronomy and Astrophysics Supplement Series, 34: 1–49, Bibcode:1978A&AS...34....1N.
  3. 1 2 Malkov, O. Yu.; et al. (2012), "Dynamical Masses of a Selected Sample of Orbital Binaries", Astronomy & Astrophysics, 546: 5, Bibcode:2012A&A...546A..69M, doi:10.1051/0004-6361/201219774, A69
  4. 1 2 3 Royer, F.; et al. (February 2007), "Rotational velocities of A-type stars. III. Velocity distributions", Astronomy and Astrophysics, 463 (2): 671–682, arXiv:astro-ph/0610785, Bibcode:2007A&A...463..671R, doi:10.1051/0004-6361:20065224.
  5. 1 2 Cvetkovic, Z.; Ninkovic, S. (2010), "On the Component Masses of Visual Binaries", Serbian Astronomical Journal, 180: 71–80, Bibcode:2010SerAJ.180...71C, doi:10.2298/SAJ1080071C.
  6. ↑ de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: 14, arXiv:1208.3048, Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, A61.
  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.
  8. 1 2 3 Tokovinin, Andrei; et al. (August 2015), "Speckle Interferometry at SOAR in 2014", The Astronomical Journal, 150 (2): 17, arXiv:1506.05718, Bibcode:2015AJ....150...50T, doi:10.1088/0004-6256/150/2/50, 50.
  9. 1 2 3 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.
  10. 1 2 Beers, T. C.; et al. (February 2001), "Metallicity estimates for A-, F-, and G-type stars from the Edinburgh-Cape Blue Object Survey", Monthly Notices of the Royal Astronomical Society, 320 (4): 451−464, arXiv:astro-ph/0011491, Bibcode:2001MNRAS.320..451B, doi:10.1046/j.1365-8711.2001.03952.x.
  11. ↑ "psi Crt -- Double or multiple star", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg, retrieved 2017-02-26.
  12. ↑ Murphy, Simon J.; et al. (October 2015), "An Evaluation of the Membership Probability of 212 λ Boo Stars. I. A Catalogue", Publications of the Astronomical Society of Australia, 32: 43, arXiv:1508.03633, Bibcode:2015PASA...32...36M, doi:10.1017/pasa.2015.34, e036.
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