HD 177565

Last updated
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">3 Piscis Austrini</span> Star in the constellation Microscopium

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<span class="mw-page-title-main">HD 193307</span> Star in the constellation Telescopium

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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

HD 76236, also designated as HR 3543 or rarely 11 G. Chamaeleontis, is a solitary star located in the southern circumpolar constellation Chamaeleon. It is faintly visible to the naked eye as an orange-hued star with an apparent magnitude of 5.77. Based on parallax measurements from the Gaia satellite, the object is estimated to be 612 light years away. Currently, it is receding with a heliocentric radial velocity of 7 km/s. At its current distance, HD 76236's brightness is diminished by 0.39 magnitudes due to interstellar dust. It has an absolute magnitude of −0.13.

HD 37289, also known as HR 1916, is a solitary, orange hued star located in the northern circumpolar constellation Camelopardalis. It has an apparent magnitude of 5.61, making it faintly visible to the naked eye under ideal conditions. Based on parallax measurements from the Gaia spacecraft, the object is estimated to be 308 light years distant. It appears to be approaching the Sun, having a heliocentric radial velocity of −20.7 km/s.

HD 58425, also known as HR 2830, is an astrometric binary located in the northern circumpolar constellation Camelopardalis. It is faintly visible to the naked eye as an orang point of light at an apparent magnitude of 5.64. Based on parallax measurements from Gaia DR3, the system is estimated to be 470 light years away from Earth. It appears to be rapidly receding from the Sun, having a heliocentric radial velocity of 58.6 km/s. HD 58425 is listed as 54 Ursae Majoris in Johann Hevelius' catalogue, but this was dropped after the official IAU's official constellation borders were drawn.

HD 31529, also known as HR 1584, is a solitary, orange hued star located in the southern constellation Caelum, the chisel. It has an apparent magnitude of 6.09, making it faintly visible to the naked eye if viewed under ideal conditions. This object is located relatively far at a distance of 932 light years based on parallax measurements from Gaia DR3, but is receding with a heliocentric radial velocity of 28.4 km/s. Eggen (1989) lists it as a member of the old disk population.

HD 32820, also known as HR 1651, is a yellowish-white hued star located in the southern constellation Caelum, the chisel. It has an apparent magnitude of 6.3, placing it near the limit of naked eye visibility. The object is located relatively close at a distance of 103 light years based on parallax measurements from Gaia DR3, but is receding with a heliocentric radial velocity of 29.8 km/s.

<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 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.

References

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  7. 1 2 Ramírez, I.; Fish, J. R.; Lambert, D. L.; Allende Prieto, C. (13 August 2012). "Lithium Abundances in nearby FGK Dwarf and Subgiant Stars: Internal Destruction, Galactic Chemical Evolution, and Exoplanets". The Astrophysical Journal. 756 (1): 46. arXiv: 1207.0499 . Bibcode:2012ApJ...756...46R. doi: 10.1088/0004-637X/756/1/46 . eISSN   1538-4357. ISSN   0004-637X. S2CID   119199829.
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  9. ↑ Aguilera-Gómez, Claudia; Ramírez, Iván; Chanamé, Julio (June 2018). "Lithium abundance patterns of late-F stars: an in-depth analysis of the lithium desert". Astronomy & Astrophysics. 614: A55. arXiv: 1803.05922 . Bibcode:2018A&A...614A..55A. doi: 10.1051/0004-6361/201732209 . eISSN   1432-0746. ISSN   0004-6361. S2CID   62799777.
  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.
  11. 1 2 Nordström, B.; Mayor, M.; Andersen, J.; Holmberg, J.; Pont, F.; Jørgensen, B. R.; Olsen, E. H.; Udry, S.; Mowlavi, N. (16 April 2004). "The Geneva-Copenhagen survey of the Solar neighbourhood". Astronomy & Astrophysics. 418 (3): 989–1019. arXiv: astro-ph/0405198 . Bibcode:2004A&A...418..989N. doi: 10.1051/0004-6361:20035959 . eISSN   1432-0746. ISSN   0004-6361. S2CID   11027621.
  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. 836 (1). American Astronomical Society: 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.
  18. ↑ Evans, D. S.; Menzies, A.; Stoy, R. H. (1 December 1959). "Fundamental Data for Southern Stars (Second List)". Monthly Notices of the Royal Astronomical Society. 119 (6): 638–647. Bibcode:1959MNRAS.119..638E. doi: 10.1093/mnras/119.6.638 . eISSN   1365-2966. ISSN   0035-8711.
  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. 470 (4). Oxford University Press (OUP): 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. 661. EDP Sciences: A23. arXiv: 2106.14550 . Bibcode:2022A&A...661A..23F. doi: 10.1051/0004-6361/202141097 . ISSN   0004-6361.
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