HD 107146

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HD 107146
HD 107146 falsecolour.jpg
False colour image of HD 107146 taken by the Hubble Space Telescope, showing its circumstellar disc. The right side of the disc is brighter—this is thought to be because it is closer to the Earth.
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Coma Berenices
Right ascension 12h 19m 06.50230s[1]
Declination 16° 32′ 53.8628″[1]
Apparent magnitude (V) 7.028[2]
Spectral type G2V[3]
U−B color index +0.073[2]
B−V color index +0.602[2]
Radial velocity (Rv) 1.88[4] km/s
Proper motion (μ) RA: -174.16[1] mas/yr
Dec.: -148.90[1] mas/yr
Parallax (π) 36.42 ± 0.54[1] mas
Distance 90 ± 1 ly
(27.5 ± 0.4 pc)
Mass 1.09[5] M
Radius 0.993 ± 0.014[5] R
Luminosity 1.1[6] L
Surface gravity (log g) 4.56[7] cgs
Temperature 5,850[5] K
Metallicity [Fe/H] 0.00[7] dex
Rotation 3.50 ± 1.35 days[5]
Age 80–200 myr[8] years
Other designations
BD+17 2462, NLTT 30317, SAO 100038, HD 107146, HIP 60074.[3]

HD 107146 is a star in the constellation Coma Berenices that is located about 90 light years from Earth.[8] The apparent magnitude of 7.028 makes this star too faint to be seen with the unaided eye.

The physical properties of this star are similar to the Sun, including the stellar classification G2V,[3] making this a solar analog.[9] The mass of this star is about 109% of the solar mass (M) and it has about 99% the radius of the Sun (R).[5] It is a young star with an age between 80 and 200 Myr.[8] The axis of rotation is estimated at 21+8
degrees to the line of sight and it completes a rotation in a relatively brief 3.5 days.[5]

Circumstellar disc[edit]

In 2003, astronomers recognized the excess infrared[10] and submillimeter[8] emission indicative of circumstellar dust, the first time such a debris disk phenomenon was noted around a star of similar spectral types to the Sun, though having a much younger age. In 2004 the Hubble Space Telescope detected the presence of a spatially resolved disk surrounding the star[6][11]

The star's circumstellar disc has dimensions of approximately 210 x 300 AU.[8] The dusty ring is cool, with a temperature of 51 K, and has a mass of 0.10 Earth masses (M).[8] Analysis of the debris disk in the far-infrared and submillimeter wavelengths, carried out using the Hubble Space Telescope, suggests the presence of small grains in the disk.[6] The disk appears to be slightly elongated to form an ellipse with its minor axis at a position angle of 58° ± 5°; working under the assumption that the disk is in fact circular gives it an inclination of 25° ± 5° from the plane of the sky.[6] An analysis published in 2009 suggests the possible presence of a planet at a separation of 45-75 AU.[9]


  1. ^ a b c d e van Leeuwen, F. (November 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. 
  2. ^ a b c Landolt, A. U. (June 1983), "UBVRI photometry of stars useful for checking equipment orientation stability", Astronomical Journal 88: 853–866, Bibcode:1983AJ.....88..853L, doi:10.1086/113372 
  3. ^ a b c "HD 107146". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2011-12-14. 
  4. ^ White, Russel J. et al. (June 2007), "High-dispersion optical spectra of nearby stars younger than the Sun", The Astronomical Journal 133 (6): 2524–2536, arXiv:0706.0542, Bibcode:2007AJ....133.2524W, doi:10.1086/514336 
  5. ^ a b c d e f Watson, C. A. et al. (May 2011). "On the alignment of debris discs and their host stars' rotation axis - implications for spin-orbit misalignment in exoplanetary systems". Monthly Notices of the Royal Astronomical Society: Letters 413 (1): L71–L75. arXiv:1009.4132. Bibcode:2011MNRAS.413L..71W. doi:10.1111/j.1745-3933.2011.01036.x. 
  6. ^ a b c d Ardila, D. R. et al. (2004). "A resolved debris disk around the G2 V star HD 107146". The Astrophysical Journal, Part 2 617: L147–L150. arXiv:astro-ph/0411422. Bibcode:2004ApJ...617L.147A. doi:10.1086/427434. 
  7. ^ a b Brugamyer, Erik et al. (September 2011). "Silicon and Oxygen Abundances in Planet-host Stars". The Astrophysical Journal 738 (1). arXiv:1106.5509. Bibcode:2011ApJ...738...97B. doi:10.1088/0004-637X/738/1/97. 
  8. ^ a b c d e f Williams, Jonathan P. et al. (March 2004). "Detection of cool dust around the G2 V star HD 107146". The Astrophysical Journal 604: 414–419. arXiv:astro-ph/0311583. Bibcode:2004ApJ...604..414W. doi:10.1086/381721. 
  9. ^ a b Corder, S. A. et al. (2009). "A resolved ring of debris dust around the solar analog HD 107146". The Astrophysical Journal 690: L65–L68. arXiv:0811.2713. Bibcode:2009ApJ...690L..65C. doi:10.1088/0004-637X/690/1/L65. 
  10. ^ Metchev, Stanimir A.; Hillenbrand, Lynne A.; Meyer, Michael R. (January 2004). "Ten micron observations of nearby young stars". The Astrophysical Journal 600: 435–450. arXiv:astro-ph/0309453. Bibcode:2004ApJ...600..435M. doi:10.1086/379788. 
  11. ^ "Spitzer and Hubble capture evolving planetary systems". hubblesite.org. December 9, 2004. Retrieved 2011-12-14.