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HD 15115

Debris disk surrounding young star HD 15115
Credit: NASA
Observation data
Epoch J2000       Equinox J2000
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  mas [1]
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
SIMBAD data

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. ^ a b c d e f g h i j k l Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv: 1804.09365. Bibcode: 2018A&A...616A...1G. doi: 10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. ^ a b c d Oja, T. (1983). "UBV photometry of FK4 and FK4 supplement stars". Astronomy and Astrophysics Supplement Series. 52: 131. Bibcode: 1983A&AS...52..131O.
  3. ^ a b Harlan, E. A. (1974). "MK classification for F- and G-type stars. III". Astronomical Journal. 79: 682. Bibcode: 1974AJ.....79..682H. doi: 10.1086/111597.
  4. ^ a b c MacGregor, Meredith A.; et al. (March 2015). "Resolved Millimeter Emission from the HD 15115 Debris Disk". The Astrophysical Journal. 801 (1): 8. arXiv: 1501.05962. Bibcode: 2015ApJ...801...59M. doi: 10.1088/0004-637X/801/1/59. S2CID  118407532. 59.
  5. ^ a b 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. arXiv: 1405.1559. Bibcode: 2015A&A...573A.126D. doi: 10.1051/0004-6361/201323168. S2CID  55486025. A126.
  6. ^ a b c d e Luck, R. Earle (March 2018), "Abundances in the Local Region. III. Southern F, G, and K Dwarfs", The Astronomical Journal, 155 (3): 31, Bibcode: 2018AJ....155..111L, doi: 10.3847/1538-3881/aaa9b5, S2CID  125765376, 111.
  7. ^ a b Pribulla, Theodor; et al. (September 2014). "Cerro Armazones spectroscopic survey of F dwarfs". Monthly Notices of the Royal Astronomical Society. 443 (3): 2815–2823. Bibcode: 2014MNRAS.443.2815P. doi: 10.1093/mnras/stu1333.
  8. ^ a b Decin, G.; et al. (November 2003), "Age Dependence of the Vega Phenomenon: Observations", The Astrophysical Journal, 598 (1): 636–644, arXiv: astro-ph/0308294, Bibcode: 2003ApJ...598..636D, doi: 10.1086/378800, S2CID  16751327
  9. ^ "HD 15115". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-11-15.
  10. ^ Rodriguez, David R.; Zuckerman, B. (February 2012). "Binaries among Debris Disk Stars". The Astrophysical Journal. 745 (2): 13. arXiv: 1111.5618. Bibcode: 2012ApJ...745..147R. doi: 10.1088/0004-637X/745/2/147. S2CID  73681879. 147.
  11. ^ a b 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. arXiv: 1508.06929. Bibcode: 2015A&A...583A..85A. doi: 10.1051/0004-6361/201526795. S2CID  3131908. A85.
  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, arXiv: 1209.2077, Bibcode: 2013ApJ...762...88M, doi: 10.1088/0004-637X/762/2/88, S2CID  118497872, 88.
  13. ^ Debes, J. H.; et al. (2009). "Interstellar Medium Sculpting of the Hd 32297 Debris Disk". The Astrophysical Journal. 702 (1): 318–326. arXiv: 0908.4368. Bibcode: 2009ApJ...702..318D. doi: 10.1088/0004-637X/702/1/318. S2CID  15303091.
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