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HD 15115

Topic: Astronomy

 From HandWiki - Reading time: 5 min

Short description: F-type subgiant star in the constellation Cetus
HD 15115

Debris disk surrounding young star HD 15115
Credit: NASA
Observation data
Equinox J2000.0]] (ICRS)
Constellation Cetus
Right ascension  02h 26m 16.24577s[1]
Declination +06° 17′ 33.1880″[1]
Apparent magnitude (V) 6.76[2]
Characteristics
Spectral type F4IV[3] or F2V[4]
U−B color index −0.03[2]
B−V color index +0.39[2]
Astrometry
Radial velocity (Rv)0.81±0.12[5] km/s
Proper motion (μ) RA: +88.030[1] mas/yr
Dec.: -50.515[1] mas/yr
Parallax (π)20.4065 ± 0.0418[1] mas
Distance159.8 ± 0.3 ly
(49.0 ± 0.1 pc)
Details
Mass1.19[6] M☉
Radius1.39±0.06[1] R☉
Luminosity3.74±0.01[1] L☉
Surface gravity (log g)4.30[6] cgs
Temperature6,811+148
−152[1] K
Metallicity [Fe/H]0.96[6] dex
Rotational velocity (v sin i)89.8[7] km/s
Age500[8] Myr
Other designations
BD+05°338, HD 15115, HIP 11360, SAO 110532, WDS J02263+0618A[9]
Database references
SIMBADdata

HD 15115 is a single[10] star in the equatorial constellation of Cetus. It is readily visible in binoculars or a small telescope, but is considered too dim to be seen with the naked eye at an apparent visual magnitude of 6.76.[2] The distance to this object is 160 light years based on parallax,[1] and it is slowly drifting further away at the rate of about 1 km/s.[5] It has been proposed as a member of the Beta Pictoris moving group[11] or the Tucana-Horologium association of co-moving stars; there is some ambiguity as to its true membership.[12]

This object has a stellar classification of F4IV,[3] suggesting it is an aging subgiant star that has exhausted the supply of hydrogen at its core. MacGregor and associates (2015) instead classify it as a young F-type main-sequence star with a class of F2V.[4] Age estimates give a value of 500[8] million years, while membership in the β Pictoris moving group would indicate an age of around 21±4 million.[4] It has 1.19[6] times the mass of the Sun, 1.39[1] times the Sun's radius, and has a relatively high rate of spin with a projected rotational velocity of 90 km/s.[7] The star is radiating 3.74[1] times the luminosity of the Sun from its photosphere at an effective temperature of 6,811 K.[1] Its metallicity – the abundance of elements other than hydrogen and helium – is nearly the same as in the Sun.[6]

HD 15115 was shown to have an asymmetric debris disk surrounding it, which is being viewed nearly edge-on. The reason for the asymmetry is thought to be either the gravitational pull of a passing star (HIP 12545), an exoplanet, or interaction with the local interstellar medium.[13] A magnitude 11.35 visual companion lies at an angular separation of 12.6″ along a position angle of 195°, as of 2015.[11]

References

  1. ↑ 1.00 1.01 1.02 1.03 1.04 1.05 1.06 1.07 1.08 1.09 1.10 1.11 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G.  Gaia DR2 record for this source at VizieR.
  2. ↑ 2.0 2.1 2.2 2.3 Oja, T. (1983). "UBV photometry of FK4 and FK4 supplement stars". Astronomy and Astrophysics Supplement Series 52: 131. Bibcode: 1983A&AS...52..131O. 
  3. ↑ 3.0 3.1 Harlan, E. A. (1974). "MK classification for F- and G-type stars. III". Astronomical Journal 79: 682. doi:10.1086/111597. Bibcode: 1974AJ.....79..682H. 
  4. ↑ 4.0 4.1 4.2 MacGregor, Meredith A. et al. (March 2015). "Resolved Millimeter Emission from the HD 15115 Debris Disk". The Astrophysical Journal 801 (1): 8. doi:10.1088/0004-637X/801/1/59. 59. Bibcode: 2015ApJ...801...59M. 
  5. ↑ 5.0 5.1 Desidera, S. et al. (January 2015). "The VLT/NaCo large program to probe the occurrence of exoplanets and brown dwarfs in wide orbits. I. Sample definition and characterization". Astronomy & Astrophysics 573: 45. doi:10.1051/0004-6361/201323168. A126. Bibcode: 2015A&A...573A.126D. 
  6. ↑ 6.0 6.1 6.2 6.3 6.4 Luck, R. Earle (March 2018), "Abundances in the Local Region. III. Southern F, G, and K Dwarfs", The Astronomical Journal 155 (3): 31, doi:10.3847/1538-3881/aaa9b5, 111, Bibcode: 2018AJ....155..111L. 
  7. ↑ 7.0 7.1 Pribulla, Theodor et al. (September 2014). "Cerro Armazones spectroscopic survey of F dwarfs". Monthly Notices of the Royal Astronomical Society 443 (3): 2815–2823. doi:10.1093/mnras/stu1333. Bibcode: 2014MNRAS.443.2815P. 
  8. ↑ 8.0 8.1 Decin, G. et al. (November 2003), "Age Dependence of the Vega Phenomenon: Observations", The Astrophysical Journal 598 (1): 636–644, doi:10.1086/378800, Bibcode: 2003ApJ...598..636D 
  9. ↑ "HD 15115". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+15115. 
  10. ↑ Rodriguez, David R.; Zuckerman, B. (February 2012). "Binaries among Debris Disk Stars". The Astrophysical Journal 745 (2): 13. doi:10.1088/0004-637X/745/2/147. 147. Bibcode: 2012ApJ...745..147R. 
  11. ↑ 11.0 11.1 Alonso-Floriano, F. J. et al. (November 2015). "Reaching the boundary between stellar kinematic groups and very wide binaries. III. Sixteen new stars and eight new wide systems in the β Pictoris moving group". Astronomy & Astrophysics 583: 24. doi:10.1051/0004-6361/201526795. A85. Bibcode: 2015A&A...583A..85A. 
  12. ↑ Malo, Lison et al. (January 2013), "Bayesian Analysis to Identify New Star Candidates in Nearby Young Stellar Kinematic Groups", The Astrophysical Journal 762 (2): 50, doi:10.1088/0004-637X/762/2/88, 88, Bibcode: 2013ApJ...762...88M. 
  13. ↑ Debes, J. H. et al. (2009). "Interstellar Medium Sculpting of the Hd 32297 Debris Disk". The Astrophysical Journal 702 (1): 318–326. doi:10.1088/0004-637X/702/1/318. Bibcode: 2009ApJ...702..318D. 



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