Astronomy:Chi Serpentis
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Serpens |
| Right ascension | 15h 41m 47.41474s[2] |
| Declination | +12° 50′ 51.0937″[2] |
| Apparent magnitude (V) | +5.30[3] |
| Characteristics | |
| Spectral type | A2 Vp MnEu(Sr)[4] |
| U−B color index | +0.04[3] |
| B−V color index | +0.04[3] |
| Variable type | α2 CVn[5] |
| Astrometry | |
| Radial velocity (Rv) | +1.90±1.78[6] km/s |
| Proper motion (μ) | RA: +39.045[2] mas/yr Dec.: −2.923[2] mas/yr |
| Parallax (π) | 14.7221 ± 0.0748[2] mas |
| Distance | 222 ± 1 ly (67.9 ± 0.3 pc) |
| Absolute magnitude (MV) | +1.10[7] |
| Details | |
| Mass | 2.11[8] M☉ |
| Radius | 1.9[9] R☉ |
| Luminosity | 26[10] L☉ |
| Surface gravity (log g) | 3.66±0.24[11] cgs |
| Temperature | 9,557±274[11] K |
| Metallicity [Fe/H] | +0.35±0.13[11] dex |
| Rotation | 1.5948[7] d |
| Rotational velocity (v sin i) | 75[12] km/s |
| Age | 212[8] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Chi Serpentis (χ Ser, χ Serpentis) is a solitary star[14] in the Serpens Caput section of the equatorial constellation Serpens. Based upon an annual parallax shift of 14.84 mas as seen from Earth, it is located around 222 light years from the Sun. The star is bright enough to be faintly visible to the naked eye, having an apparent visual magnitude of +5.30.[3]
In 1966 it was listed as a suspected spectroscopic binary,[15] but it is believed to be single.[14] This is a chemically peculiar star Ap star with a stellar classification of A2 Vp MnEu(Sr),[4] indicating the spectrum shows abnormal excesses of manganese and europium. The star has 2.11[8] times the mass of the Sun and about 1.9 times the Sun's radius.[9] It is radiating 26[10] times the solar luminosity from its photosphere at an effective temperature of 9,557 K.[11] At the age of 212 million years,[8] it is spinning with a rotation period of 1.6 days.[15]
Chi Serpentis is classified as an Alpha2 Canum Venaticorum type variable star,[5] and its magnitude varies by 0.03 with a period of 1.5948 days.[7] The pattern of variation in the spectrum suggest there are regions of enhanced strontium, chromium, iron, titanium, and magnesium on the surface of the star.[16] The averaged quadratic field strength of the surface magnetic field is (859.1±712.3)×10−4 T.[17]
References
- ↑ MAST: Barbara A. Mikulski Archive for Space Telescopes, Space Telescope Science Institute, https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html, retrieved 8 December 2021.
- ↑ 2.0 2.1 2.2 2.3 2.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 3.0 3.1 3.2 3.3 Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data (SIMBAD), Bibcode: 1986EgUBV........0M.
- ↑ 4.0 4.1 Loden, L. O. (July 1983), "A physical study of the Ursa Major cluster (with special attention to the peculiar A stars)", Astronomy and Astrophysics Supplement Series 53: 33–42, Bibcode: 1983A&AS...53...33L.
- ↑ 5.0 5.1 Hoffleit, D. (October 1982), "Variable stars in the General Catalogue of Trigonometric Parallaxes", Bulletin d'Information du Centre de Données Stellaires 23: 53, Bibcode: 1982BICDS..23...53H.
- ↑ 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, doi:10.1051/0004-6361/201219219, A61, Bibcode: 2012A&A...546A..61D.
- ↑ 7.0 7.1 7.2 Adelman, Saul J. (2002), "On the Periods of the Magnetic CP Stars", Baltic Astronomy 11: 475–485, Bibcode: 2002BaltA..11..475A.
- ↑ 8.0 8.1 8.2 8.3 David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal 804 (2): 146, doi:10.1088/0004-637X/804/2/146, Bibcode: 2015ApJ...804..146D.
- ↑ 9.0 9.1 Pasinetti Fracassini, L. E.; Pastori, L.; Covino, S.; Pozzi, A. (February 2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS)", Astronomy and Astrophysics 367: 521–524, doi:10.1051/0004-6361:20000451, Bibcode: 2001A&A...367..521P.
- ↑ 10.0 10.1 McDonald, I. et al. (2012), "Fundamental Parameters and Infrared Excesses of Hipparcos Stars", Monthly Notices of the Royal Astronomical Society 427 (1): 343–57, doi:10.1111/j.1365-2966.2012.21873.x, Bibcode: 2012MNRAS.427..343M.
- ↑ 11.0 11.1 11.2 11.3 Prugniel, Ph. et al. (July 2011), "The atmospheric parameters and spectral interpolator for the MILES stars", Astronomy & Astrophysics 531: A165, doi:10.1051/0004-6361/201116769, Bibcode: 2011A&A...531A.165P.
- ↑ Royer, F. et al. (October 2012), "Rotational velocities of A-type stars in the northern hemisphere. II. Measurement of v sin i", Astronomy and Astrophysics 393: 897–911, doi:10.1051/0004-6361:20020943, Bibcode: 2002A&A...393..897R.
- ↑ "chi Ser". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=chi+Ser.
- ↑ 14.0 14.1 Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society 389 (2): 869–879, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E.
- ↑ 15.0 15.1 Rajamohan, R.; Babu, G. S. D. (March 1978), "On the intrinsic rotation of magnetic variables", Monthly Notices of the Royal Astronomical Society 182 (4): 773–776, doi:10.1093/mnras/182.4.773, Bibcode: 1978MNRAS.182..773R.
- ↑ Riabchikova, T. A. (February 1975), "The spectroscopic variable AP star chi Serpentis", Soviet Astronomy 18: 451–453, Bibcode: 1975SvA....18..451R.
- ↑ Bychkov, V. D. et al. (April 2009), "Catalogue of averaged stellar effective magnetic fields - II. Re-discussion of chemically peculiar A and B stars", Monthly Notices of the Royal Astronomical Society 394 (3): 1338–1350, doi:10.1111/j.1365-2966.2008.14227.x, Bibcode: 2009MNRAS.394.1338B.
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