HD 177565

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HD 177565
Corona Australis constellation map.svg
Red circle.svg
Location of HD 177565 (circled)
Observation data
Epoch J2000.0        Equinox J2000.0 (ICRS)
Constellation Corona Australis
Right ascension 19h 06m 52.46439s [1]
Declination −37° 48′ 38.3734″ [1]
Apparent magnitude  (V)6.16 [2]
Characteristics
Spectral type G6 V [3]
U−B color index +0.27 [4]
B−V color index +0.70 [4]
Astrometry
Radial velocity (Rv)60.9±0.8 [5]  km/s
Proper motion (μ)RA: −187.700  mas/yr [1]
Dec.: −367.009  mas/yr [1]
Parallax (π)58.9860 ± 0.0376  mas [1]
Distance 55.29 ± 0.04  ly
(16.95 ± 0.01  pc)
Absolute magnitude  (MV)+5.00 [6]
Details
Mass 0.99+0.03
−0.04 [7]   M☉
Radius 0.985±0.022 [8]   R☉
Luminosity 0.851±0.005 [1]   L☉
Surface gravity (log g)4.44±0.03 [9]   cgs
Temperature 5,627±19 [10]   K
Metallicity [Fe/H]0.08±0.01 [10]   dex
Rotational velocity (v sin i)3 [11]  km/s
Age 4.58±1.51 [12]   Gyr
Other designations
42 G. Coronae Australis [13] , CD−37°13049, CPD−37°8466, GC  26283, GJ  744, HD  177565, HIP  93858, HR  7232, SAO  210937, LTT  7569 [14]
Database references
SIMBAD data

HD 177565 (HR 7232; LTT 7569; Gliese 744) is a yellow-hued star located in the southern constellation Corona Australis. It has an apparent magnitude of 6.16, [2] placing it near the limit for naked eye visibility, even under ideal conditions. The object is located relatively close at a distance of 55.3 light-years based on Gaia DR3 parallax measurements, [1] but it is receding rapidly with a heliocentric radial velocity of 60.9  km/s . [5] At its current distance, HD 177565's brightness is diminished by interstellar extinction of 0.07 magnitudes [15] and it as an absolute magnitude of +5.00. [6] A 2017 multiplicity survey failed to detect any stellar companions around the star. [16]

HD 177565 has a stellar classification of G6 V, [3] indicating that it is an ordinary G-type main-sequence star like our Sun. The object has also be given a later class of G8 V (Houk 1982) [17] and one source lists it as a G5 subgiant. [18] It has 99% the mass of the Sun [7] and 98.5% the Sun's radius. [8] It radiates 85.1% the luminosity of the Sun [1] from its photosphere at an effective temperature of 5,627  K , [10] making it slightly cooler than the Sun. HD 177565 is slightly metal enriched with an iron abundance at [Fe/H] = +0.08 (120% solar) [10] and it is estimated to be 4.58 billion years old. [12] HD 177565 spins slightly faster than the Sun with a projected rotational velocity of 3  km/s [11] compared to the Sun's rotational velocity of 2 km/s.

Planetary system

In 2017, an exoplanet was discovered orbiting the star after observations of HARPS data. HD 177565 b is a hot Neptune that takes 44.5 days to revolve around its host star in a relatively circular orbit. [19]

The HD 177565 planetary system [19]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b≥15.10+6.40
−6.05  M🜨 		0.246±0.01944.5+0.6
−0.3		0.059+0.172
−0.058		—~4.1 [20]   R🜨

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<span class="mw-page-title-main">HD 201772</span> Star in the constellation Microscopium

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<span class="mw-page-title-main">HD 117566</span> High proper motion star; Camelopardalis

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<span class="mw-page-title-main">HD 168592</span> Star in the constellation of Corona Australis

HD 168592, also designated as HR 6862 or rarely 7 G. Coronae Australis, is a solitary star located in the southern constellation Corona Australis. It is faintly visible to the naked eye as an orange-hued star with an apparent magnitude of 5.07. Gaia DR3 parallax measurements place it at a distance of 490 light years and is currently receding with a heliocentric radial velocity of 18 km/s. At its current distance, HD 168592's brightness is diminished by 0.38 magnitudes due to interstellar dust. It has an absolute magnitude of −0.76.

<span class="mw-page-title-main">HD 31134</span> Star in the constellation of Camelopardalis

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References

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  10. 1 2 3 4 Sousa, S. G.; Santos, N. C.; Mayor, M.; Udry, S.; Casagrande, L.; Israelian, G.; Pepe, F.; Queloz, D.; Monteiro, M. J. P. F. G. (4 June 2008). "Spectroscopic parameters for 451 stars in the HARPS GTO planet search program". Astronomy & Astrophysics. 487 (1): 373–381. arXiv: 0805.4826 . Bibcode:2008A&A...487..373S. doi: 10.1051/0004-6361:200809698 . eISSN   1432-0746. ISSN   0004-6361. S2CID   18173201.
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  12. 1 2 Gomes da Silva, J.; Santos, N. C.; Adibekyan, V.; Sousa, S. G.; Campante, T. L.; Figueira, P.; Bossini, D.; Delgado-Mena, E.; Monteiro, M. J. P. F. G.; de Laverny, P.; Recio-Blanco, A.; Lovis, C. (February 2021). "Stellar chromospheric activity of 1674 FGK stars from the AMBRE-HARPS sample. I. A catalogue of homogeneous chromospheric activity". Astronomy & Astrophysics. 646: A77. arXiv: 2012.10199 . Bibcode:2021A&A...646A..77G. doi: 10.1051/0004-6361/202039765 . eISSN   1432-0746. ISSN   0004-6361. S2CID   229331727.
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  16. ↑ Fuhrmann, K.; Chini, R.; Kaderhandt, L.; Chen, Z. (February 14, 2017). "Multiplicity among Solar-type Stars". The Astrophysical Journal. American Astronomical Society. 836 (1): 139. Bibcode:2017ApJ...836..139F. doi: 10.3847/1538-4357/836/1/139 . ISSN   1538-4357. S2CID   125253901.
  17. ↑ 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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  19. 1 2 Feng, F.; Tuomi, M.; Jones, H. R. A. (May 16, 2017). "Agatha: disentangling periodic signals from correlated noise in a periodogram framework". Monthly Notices of the Royal Astronomical Society. Oxford University Press (OUP). 470 (4): 4794–4814. arXiv: 1705.03089 . Bibcode:2017MNRAS.470.4794F. doi: 10.1093/mnras/stx1126 . ISSN   0035-8711. S2CID   73635720.
  20. ↑ Foster, G.; Poppenhaeger, K.; Ilic, N.; Schwope, A. (2022). "Exoplanet X-ray irradiation and evaporation rates with eROSITA". Astronomy & Astrophysics. EDP Sciences. 661: A23. arXiv: 2106.14550 . Bibcode:2022A&A...661A..23F. doi: 10.1051/0004-6361/202141097 . ISSN   0004-6361.
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