Psi Crateris

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.

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

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. 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. 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. 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. 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. 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. 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. 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. 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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