Astronomy:Eta Scorpii
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| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Scorpius |
| Right ascension | 17h 12m 09.19565s[1] |
| Declination | –43° 14′ 21.0905″[1] |
| Apparent magnitude (V) | 3.33[2] |
| Characteristics | |
| Spectral type | F5 IV[3] |
| U−B color index | +0.09[2] |
| B−V color index | +0.41[2] |
| Astrometry | |
| Radial velocity (Rv) | –27.0[4] km/s |
| Proper motion (μ) | RA: +24.47[1] mas/yr Dec.: –288.55[1] mas/yr |
| Parallax (π) | 44.39 ± 0.16[1] mas |
| Distance | 73.5 ± 0.3 ly (22.53 ± 0.08 pc) |
| Absolute magnitude (MV) | +1.58[5] |
| Details[6] | |
| Mass | 1.75[7] M☉ |
| Radius | 3.307±0.050 R☉ |
| Luminosity | 17.94±0.45 L☉ |
| Surface gravity (log g) | 3.65±0.20 cgs |
| Temperature | 6,533±46 K |
| Metallicity [Fe/H] | −0.29±0.10 dex |
| Rotational velocity (v sin i) | 150.00 km/s |
| Age | 1.1[5] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Eta Scorpii, Latinized from η Scorpii, is a star in the southern zodiac constellation of Scorpius. With an apparent visual magnitude of 3.33,[2] this is one of the brighter members of the Scorpius and is the furthest south of the constellation stars with a Bayer designation.[9] The distance to this star can be estimated using parallax measurements, yielding a value of 73.5 light-years (22.5 parsecs) with a 0.4% margin of error.[1]
The stellar classification of this star has undergone some revision over time, with the star being classified anywhere from an F-type main sequence star to a giant star.[8] In 2006, the NStars program assigned it a class of F5 IV,[3] where the luminosity class of 'IV' indicates this is a subgiant star that is exhausting the supply of hydrogen at its core and is in the process of evolving into a giant star. It has around 175%[7] of the Sun's mass with an estimated age of 1.1 billion years.[5] The star is radiating about 18 times the luminosity of the Sun from its outer atmosphere at an effective temperature of 6,533 K.[6] It is this heat that gives it a yellow-white hue that is typical for an F-type star.[10]
Eta Scorpii is rotating rapidly, with a projected rotational velocity of 150 km s−1.[7] This is causing the star to spin on its axis with a period of less than a day.[11] It is an X-ray emitter with its stellar corona giving off an X-ray luminosity of 4.4×1028 ergs s−1.[12] In 1991 it was identified as a possible barium star, as it displays an enhanced abundance of the element barium in its spectrum.[13] Overall, the abundance of elements other than hydrogen and helium, what astronomers term the star's metallicity, is similar to the abundance in the Sun.[5]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V
- ↑ 2.0 2.1 2.2 2.3 Bok, B. J.; Bok, P. F.; Miller, E. W. (November 1972), "Photometric standards for the southern hemisphere. II", Astronomical Journal 77: 733, doi:10.1086/111346, Bibcode: 1972AJ.....77..733B
- ↑ 3.0 3.1 Gray, R. O. et al. (July 2006), "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 pc-The Southern Sample", The Astronomical Journal 132 (1): 161–170, doi:10.1086/504637, Bibcode: 2006AJ....132..161G
- ↑ Evans, D. S. (June 20–24, 1966), "The Revision of the General Catalogue of Radial Velocities", in Batten, Alan Henry; Heard, John Frederick, Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30, University of Toronto: International Astronomical Union, Bibcode: 1967IAUS...30...57E
- ↑ 5.0 5.1 5.2 5.3 Holmberg, J.; Nordstrom, B.; Andersen, J. (July 2009). "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics". Astronomy and Astrophysics 501 (3): 941–947. doi:10.1051/0004-6361/200811191. Bibcode: 2009A&A...501..941H.
- ↑ 6.0 6.1 Rains, Adam D. et al. (April 2020), "Precision angular diameters for 16 southern stars with VLTI/PIONIER", Monthly Notices of the Royal Astronomical Society 493 (2): 2377–2394, doi:10.1093/mnras/staa282, Bibcode: 2020MNRAS.493.2377R
- ↑ 7.0 7.1 7.2 Mallik, Sushma V.; Parthasarathy, M.; Pati, A. K. (October 2003), "Lithium and rotation in F and G dwarfs and subgiants", Astronomy and Astrophysics 409: 251–261, doi:10.1051/0004-6361:20031084, Bibcode: 2003A&A...409..251M
- ↑ 8.0 8.1 "LTT 6848 -- High proper-motion Star", SIMBAD (Centre de Données astronomiques de Strasbourg), http://simbad.u-strasbg.fr/simbad/sim-id?Ident=Eta+Scorpii, retrieved 2012-02-10
- ↑ Burnham, Robert (1978), Burnham's celestial handbook: an observer's guide to the universe beyond the solar system, Dover books explaining science, 3 (2nd ed.), Courier Dover Publications, p. 1675, ISBN 0-486-23673-0, https://books.google.com/books?id=PJzIt3SIlkUC&pg=PA1675
- ↑ "The Colour of Stars", Australia Telescope, Outreach and Education (Commonwealth Scientific and Industrial Research Organisation), December 21, 2004, http://outreach.atnf.csiro.au/edu, retrieved 2012-02-10
- ↑ Kaler, James B., "Eta Scorpii", Stars (University of Illinois), http://stars.astro.illinois.edu/sow/etasco.html, retrieved 2012-02-10
- ↑ Pizzolato, N.; Maggio, A.; Sciortino, S. (September 2000), "Evolution of X-ray activity of 1-3 Msun late-type stars in early post-main-sequence phases", Astronomy and Astrophysics 361: 614–628, Bibcode: 2000A&A...361..614P
- ↑ Lu, Phillip K. (June 1991), "Taxonomy of barium stars", Astronomical Journal 101: 2229–2254, doi:10.1086/115845, Bibcode: 1991AJ....101.2229L
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