HD 201772

Last updated
HD 201772
Microscopium constellation map.svg
Red circle.svg
HD 201772 is the star circled in red
Observation data
Epoch J2000.0        Equinox J2000.0 (ICRS)
Constellation Microscopium
Right ascension 21h 13m 03.06827s [1]
Declination −39° 25 29.7097 [1]
Apparent magnitude  (V)5.26 [2]
Characteristics
Spectral type F5 IV-V [3] or F6 V Fe−0.9 CH−0.5 [4]
B−V color index +0.44 [2]
Astrometry
Radial velocity (Rv)−41±1 [5]  km/s
Proper motion (μ)RA: +185.855  mas/yr [1]
Dec.: −113.449  mas/yr [1]
Parallax (π)29.2823 ± 0.0827  mas [1]
Distance 111.4 ± 0.3  ly
(34.15 ± 0.10  pc)
Absolute magnitude  (MV)+2.66 [6]
Details
Mass 1.5 [1]   M
Radius 2.18±0.09 [7]   R
Luminosity 7.83±0.04 [1]   L
Surface gravity (log g)3.91±0.09 [8]   cgs
Temperature 6,519±80 [9]   K
Metallicity [Fe/H]−0.18±0.03 [10]   dex
Rotational velocity (v sin i)10 [11]  km/s
Age 2.23±0.04  Gyr
Other designations
56 G. Microscopii [12] , CD−39°14152, CPD−39°8898, GC  29640, HD  201772, HIP  104738, HR  8104, SAO  212793, LTT  8413 [13]
Database references
SIMBAD data

HD 201772, also known as HR 8104, is a yellowish-white hued star located in the southern constellation Microscopium. It has an apparent magnitude of 5.26, [2] making it one of the brighter members of this generally faint constellation. The object is located relatively close at a distance of 111 light-years based on Gaia DR3 parallax measurements [1] but is approaching closer with a heliocentric radial velocity of −41  km/s . [5] At its current distance, HD 201772's brightness is diminished by 0.11 magnitudes due to interstellar dust. [14]

The star has been given multiple stellar classifications over the years. It was given the luminosity class of a subgiant and main sequence star (IV/V; IV-V) [15] [3] and a dwarf (V). [16] [17] Most sources generally agree that it is a F5 star. Richard O. Gray and colleagues give HD 201772 a class of F6 V Fe−0.9 CH−0.5, which indicates that it is a F-type main-sequence star with an underabundance of iron and CH molecules in its spectrum. [4]

It has 1.47 times the mass of the Sun [18] and an enlarged radius of 2.2  R. [7] It radiates 7.8 times the luminosity of the Sun from its photosphere at an effective temperature of 6,519  K . [9] At an age of 2.5 billion years, HD 201722 is currently 1.33 magnitudes above the ZAMS, consistent with a star that is evolving off the main sequence. [11] The star has an iron abundance 66% that of the Sun, [10] making it metal deficient. It spins modestly with a projected rotational velocity of 10  km/s . [11]

HD 201772 is suspected to be a spectroscopic binary consisting of the subgiant described above and an ordinary F6 V star with a mass of 1.31  M. [19] However, the stars have no separation or an orbital period. [20] This is because the companion might be a result of spectrum contamination, so HD 201772 is more likely to be a solitary star. [21]

Related Research Articles

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<span class="mw-page-title-main">HD 24479</span> Star in the constellation Camelopardalis

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<span class="mw-page-title-main">HD 203842</span> Star in the constellation Equuleus

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<span class="mw-page-title-main">HD 26764</span> Star in the constellation Camelopardalis

HD 26764, also known as HR 1314 or rarely 14 H. Camelopardalis, is a solitary white hued star located in the northern circumpolar constellation Camelopardalis. It has an apparent magnitude of 5.19, making it faintly to the naked eye if viewed under good conditions. Gaia DR3 parallax measurements place the object at a distance of 266 light years and is drifting closer with a poorly constrained heliocentric radial velocity of 3 km/s. At its current distance, HD 26764's brightness is diminished by 0.26 magnitudes due to interstellar dust.

<span class="mw-page-title-main">HD 193307</span> High proper motion star; Telescopium

HD 193307 is the primary of a binary star located the southern constellation Telescopium. It has an apparent magnitude of 6.27, placing it near the limit for naked eye visibility, even under ideal conditions. The star is located relatively close at a distance of 102 light years based on Gaia DR3 parallax measurements, but it is receding with a heliocentric radial velocity of 16.9 km/s. At its current distance, HD 193307's brightness is diminished by 0.18 magnitudes due to extinction from interstellar dust and it has an absolute magnitude of +3.80. HD 193307 has a relatively high proper motion, moving at a rate of 437 mas/yr.

HD 28454, also known as HR 1418, is a solitary, yellowish-white hued star located in the southern constellation Caelum, the chisel. It has an apparent magnitude of 6.1, making it faintly visible to the naked eye under ideal conditions. This star is located relatively close at a distance of about 107 light years based on parallax measurements of Gaia DR3 but is receding with a heliocentric radial velocity of 15 km/s.

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

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HD 208741, also known as HR 8380, is a yellowish-white hued star located in the southern circumpolar constellation Octans. It has an apparent magnitude of 5.91, making it faintly visible to the naked eye. Parallax measurements place it at a distance of 211 light years, and it is currently receding with a heliocentric radial velocity of 8 km/s.

HD 26670, also known as HR 1305, is a star located in the northern circumpolar constellation of Camelopardalis, the giraffe. The object has been designated as 26 H. Camelopardalis, but is not commonly used in modern times. It has an apparent magnitude of 5.70, allowing it to be faintly visible to the naked eye. Based on parallax measurements from Gaia DR3, the object is estimated to be 491 light years away from the Solar System. It appears to be slowly receding with a heliocentric radial velocity of 0.4 km/s.

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<span class="mw-page-title-main">HD 198716</span> Star in the constellation of Microscopium

HD 198716, also known as HR 7987 or 33 G. Microscopii, is a solitary star located in the southern constellation Microscopium. Eggen (1993) lists it as a member of the Milky Way's old disk population.

<span class="mw-page-title-main">HD 22764</span> Double star; Camelopardalis

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<span class="mw-page-title-main">HD 204018</span> Visual binary in Microscopium

HD 204018, also designated as HR 8202, is a visual binary located in the southern constellation Microscopium. The primary has an apparent magnitude of 5.58, making it faintly visible to the naked eye under ideal conditions. The companion has an apparent magnitude of 8.09. The system is located relatively close at a distance of 176 light years based on Gaia DR3 parallax measurements but is receding with a heliocentric radial velocity of 18.3 km/s. At its current distance, HD 204018's combined brightness is diminished by 0.13 magnitudes due to interstellar dust.

HD 202908, also known as HIP 105200, is a triple star located in the equatorial constellation Equuleus. It has an apparent magnitude of 7.01, making it readily visible in binoculars but not to the naked eye. When resolved, the components have apparent magnitudes of 7.25 and 8.87 respectively. The system is located relatively close at a distance of 169 light years based on Gaia DR3 parallax measurements but it is receding with a heliocentric radial velocity of 6.24 km/s.

References

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