Summary
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.
| 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 mas[1] |
| Distance | approx. 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 | |
| Luminosity | 75[9] L☉ |
| Surface gravity (log g) | 3.8[10] cgs |
| Temperature | 9,199[9] K |
| Metallicity [Fe/H] | 0.0[10] dex |
| Rotational velocity (v sin i) | 33[4] km/s |
| Other designations | |
| Database references | |
| SIMBAD | ψ 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 edit
- ^ 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.
- ^ a b c 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.
- ^ a b 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
- ^ a b c 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, S2CID 18475298.
- ^ a b Cvetkovic, Z.; Ninkovic, S. (2010), "On the Component Masses of Visual Binaries", Serbian Astronomical Journal, 180 (180): 71–80, Bibcode:2010SerAJ.180...71C, doi:10.2298/SAJ1080071C.
- ^ 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, S2CID 59451347, A61.
- ^ 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.
- ^ a b c 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, S2CID 30737411, 50.
- ^ a b c 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.
- ^ a b 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, S2CID 119078533.
- ^ "psi Crt -- Double or multiple star", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg, retrieved 2017-02-26.
- ^ 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, S2CID 59405545, e036.