HD 170773

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HD 170773
Corona Australis constellation map.svg
Red circle.svg
Location of HD 170773 on the map (circled)
Observation data
Epoch J2000.0        Equinox J2000.0 (ICRS)
Constellation Corona Australis
Right ascension 18h 33m 00.91673s [1]
Declination −39° 53′ 31.2751″ [1]
Apparent magnitude  (V)6.22±0.01 [2]
Characteristics
Spectral type F5 V [3] [4]
B−V color index +0.42 [5]
Astrometry
Radial velocity (Rv)−25.2±1.0 [6]  km/s
Proper motion (μ)RA: +86.353  mas/yr [1]
Dec.: −79.927  mas/yr [1]
Parallax (π)27.0749 ± 0.03  mas [1]
Distance 120.5 ± 0.1  ly
(36.93 ± 0.04  pc)
Absolute magnitude  (MV)+3.38 [7]
Details
Mass 1.30 [8]   M☉
Radius 1.43±0.07 [9]   R☉
Luminosity 3.62±0.01 [1]   L☉
Surface gravity (log g)4.21±0.04 [10]   cgs
Temperature 6,694±126 [11]   K
Metallicity [Fe/H]−0.02±0.04 [12]   dex
Rotational velocity (v sin i)67.2±6.2 [13]  km/s
Age 1.50+1.2
−0.7 [10]   Gyr
Other designations
14 G. Coronae Australis [14] , CD−39°12704, CPD−39°8118, FK5  3470, GC  25304, HD  170773, HIP  90936, HR  6948, SAO  210286, TIC  313723578
Database references
SIMBAD data

HD 170773 (HR 6948; 14 G. Coronae Australis) is a solitary star located in the southern constellation Corona Australis. It has an apparent magnitude of 6.22, [2] placing it near the limit for naked eye visibility, even under ideal conditions. The object is located relatively close at a distance of 120 light-years based on Gaia DR3 parallax measurements [1] and it is drifting closer with a heliocentric radial velocity of −25.2  km/s . [6] At its current distance, HD 170773's brightness is diminished by an interstellar extinction of 0.19 magnitudes [15] and it has an absolute magnitude of +3.38. [7]

HD 170773 has a stellar classification of F5 V, [3] [4] indicating that it is an ordinary F-type main-sequence star that is generating energy via hydrogen fusion at its core. It has also been given a classification of F5 IV, indicating that it is a slightly evolved subgiant that is ceasing hydrogen fusion at its core. It has 1.30 times the mass of the Sun [8] and 1.43 times the radius of the Sun. [9] It radiates 3.62 times the luminosity of the Sun [1] from its photosphere at an effective temperature of 6,694  K , [11] giving it the typical yellowish-white hue of a F-type star. HD 170773 has a near solar metallicity of [Fe/H] = −0.02 [12] and it is estimated to be 1.5 billion years old. [10] It spins fairly quickly with a projected rotational velocity of 67.2  km/s . [13]

The star has a debris disk located 78  AU away and it has a temperature of 43 K. [16] It was first observed in 1986 by astronomers K. Sakadane and M. Nishida in their survey of Vega-like stars due to the star displaying an infrared excess that could suggest the presence of a circumstellar disk. [17] However, the actual disk was not discovered until 2004 using the Spitzer Space Telescope. [18] There might be a second cooler disk surrounding the star, but subsequent observations have not confirmed this. [16]

Related Research Articles

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<span class="mw-page-title-main">HD 27022</span> Star in the constellation Camelopardalis

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<span class="mw-page-title-main">HD 76236</span> Star in the constellation Chamaeleon

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<span class="mw-page-title-main">HD 114533</span> Star in the constellation Chamaeleon

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HD 46588 is a star in the northern circumpolar constellation Camelopardalis. It has an apparent magnitude of 5.44, allowing it to be faintly seen with the naked eye. The object is relatively close at a distance of only 59 light years but is receding with a heliocentric radial velocity of 15 km/s.

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<span class="mw-page-title-main">HD 106248</span> Star in the constellation Chamaeleon

HD 106248, also known as HR 4649, is a solitary, orange hued star located in the southern circumpolar constellation Chamaeleon. It has an apparent magnitude of 6.34, placing it near the limit for naked eye visibility. Based on parallax measurements from Gaia DR3, the object is estimated to be 358 light years away from the Solar System. It appears to be receding with a heliocentric radial velocity of 34.5 km/s. At its current distance, HD 106248's brightness is diminished by 0.32 due to interstellar dust and Eggen (1993) lists it as a member of the old (thick) disk population.

<span class="mw-page-title-main">HD 36187</span> Star in the constellation of Columba

HD 36187, also known as HR 1835, is a solitary, bluish-white hued star located in the southern constellation Columba, the dove. It has an apparent magnitude of 5.55, making it faintly visible to the naked eye under ideal conditions. Based on parallax measurements from the Gaia spacecraft, it is estimated to be 282 light years away from the Solar System. However, it is receding rapidly with a heliocentric radial velocity of 50 km/s. At its current distance, HD 36187's brightness is diminished by 0.21 magnitude due to interstellar dust.

<span class="mw-page-title-main">HD 10390</span> B-type main-sequence star; Triangulum

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References

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  3. 1 2 Houk, N. (1982). Michigan Catalogue of Two-dimensional Spectral Types for the HD stars. Declinations −40° to −26°. Vol. 3. Bibcode:1982mcts.book.....H.
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  5. ↑ Corben, P. M. (1966). "Photoelectric magnitudes and colours for bright southern stars". Monthly Notes of the Astronomical Society of South Africa. 25: 44. Bibcode:1966MNSSA..25...44C. ISSN   0024-8266.
  6. 1 2 Gontcharov, G. A. (November 2006). "Pulkovo Compilation of Radial Velocities for 35,495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759–771. arXiv: 1606.08053 . Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065. eISSN   1562-6873. ISSN   1063-7737. S2CID   119231169.
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  8. 1 2 David, Trevor J.; Hillenbrand, Lynne A. (12 May 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. arXiv: 1501.03154 . Bibcode:2015ApJ...804..146D. doi: 10.1088/0004-637X/804/2/146 . eISSN   1538-4357. S2CID   33401607.
  9. 1 2 Kervella, P.; Thévenin, F.; Di Folco, E.; Ségransan, D. (April 8, 2004). "The angular sizes of dwarf stars and subgiants: Surface brightness relations calibrated by interferometry". Astronomy & Astrophysics. 426 (1): 297–307. arXiv: astro-ph/0404180 . Bibcode:2004A&A...426..297K. doi: 10.1051/0004-6361:20035930 . eISSN   1432-0746. ISSN   0004-6361. S2CID   6077801.
  10. 1 2 3 Sepulveda, Aldo G.; Matrà, Luca; Kennedy, Grant M.; Burgo, Carlos del; Öberg, Karin I.; Wilner, David J.; Marino, Sebastián; Booth, Mark; Carpenter, John M.; Davies, Claire L.; Dent, William R. F.; Ertel, Steve; Lestrade, Jean-Francois; Marshall, Jonathan P.; Milli, Julien; Wyatt, Mark C.; MacGregor, Meredith A.; Matthews, Brenda C. (August 14, 2019). "The REASONS Survey: Resolved Millimeter Observations of a Large Debris Disk around the Nearby F Star HD 170773". The Astrophysical Journal. 881 (1): 84. arXiv: 1906.08797 . Bibcode:2019ApJ...881...84S. doi: 10.3847/1538-4357/ab2b98 . ISSN   1538-4357. S2CID   195316295.
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  14. ↑ Gould, Benjamin Apthorp (1878). "Uranometria Argentina : brillantez y posicion de las estrellas fijas, hasta la septima magnitud, comprendidas dentro de cien grados del polo austral : con atlas". Resultados del Observatorio Nacional Argentino. 1. Bibcode:1879RNAO....1.....G.
  15. ↑ Gontcharov, George A.; Mosenkov, Aleksandr V. (28 September 2017). "Verifying reddening and extinction for Gaia DR1 TGAS main sequence stars". Monthly Notices of the Royal Astronomical Society. 472 (4): 3805–3820. arXiv: 1709.01160 . Bibcode:2017MNRAS.472.3805G. doi: 10.1093/mnras/stx2219 . eISSN   1365-2966. ISSN   0035-8711. S2CID   118879856.
  16. 1 2 Moór, A.; Pascucci, I.; Kóspál, á.; Ábrahám, P.; Csengeri, T.; Kiss, L. L.; Apai, D.; Grady, C.; Henning, Th.; Kiss, Cs.; Bayliss, D.; Juhász, A.; Kovács, J.; Szalai, T. (March 2011). "Structure and Evolution of Debris Disks Around F-type Stars. I. Observations, Database, and Basic Evolutionary Aspects". The Astrophysical Journal Supplement Series. 193 (1): 4. arXiv: 1012.3631 . Bibcode:2011ApJS..193....4M. doi: 10.1088/0067-0049/193/1/4 . ISSN   0067-0049. S2CID   119243287.
  17. ↑ Sadakane, K.; Nishida, M. (July 1986). "Twelve additional 'Vega-like' stars". Publications of the Astronomical Society of the Pacific. 98: 685. Bibcode:1986PASP...98..685S. doi: 10.1086/131813 . ISSN   0004-6280. S2CID   120682699.
  18. ↑ Zuckerman, B.; Song, Inseok (March 10, 2004). "Dusty Debris Disks as Signposts of Planets: Implications for Spitzer Space Telescope". The Astrophysical Journal. 603 (2): 738–743. arXiv: astro-ph/0311546 . Bibcode:2004ApJ...603..738Z. doi: 10.1086/381700 . ISSN   0004-637X. S2CID   3456817.
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