HD 219623

Last updated
HD 219623
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Cassiopeia
Right ascension 23h 16m 42.304s [1]
Declination +53° 12′ 48.51″ [1]
Apparent magnitude  (V)5.58 [2]
Characteristics
Evolutionary stage Main sequence
Spectral type F7 V [3]
U−B color index +0.02 [4]
B−V color index +0.556±0.003 [2]
Astrometry
Radial velocity (Rv)−27.2 [5]  km/s
Proper motion (μ)RA: 112.461  mas/yr [1]
Dec.: −236.554  mas/yr [1]
Parallax (π)48.5197 ± 0.0463  mas [1]
Distance 67.22 ± 0.06  ly
(20.61 ± 0.02  pc)
Absolute magnitude  (MV)4.02 [2]
Details
Mass 1.215 [6]   M☉
Radius 1.1950±0.0359 [6]   R☉
Luminosity 1.9987±0.0265 [6]   L☉
Surface gravity (log g)4.24±0.07 [7]   cgs
Temperature 6,138±42 [7]   K
Metallicity [Fe/H]+0.07±0.03 [7]   dex
Rotational velocity (v sin i)5.50 [8]  km/s
Age 1.2 [6]   Gyr
Other designations
BD+52°3410, GJ  4324, HD  219623, HIP  114924, HR  8853, SAO  35285 [9]
Database references
SIMBAD data

HD 219623 is a solitary star in the northern circumpolar constellation of Cassiopeia. [10] HD 219623 is its Henry Draper Catalogue designation. It has an apparent visual magnitude of 5.59, [4] which lies in the brightness range that is visible to the naked eye. According to the Bortle scale, it can be observed from dark suburban skies. Parallax measurements place it at an estimated distance of around 67.2  light years. [1] It has a relatively high proper motion, advancing 262  mas per year across the celestial sphere. [11]

This star has a stellar classification of F7 V, [3] indicating that it is an F-type main-sequence star that is generating energy at its core through the thermonuclear fusion of hydrogen into helium. It is larger than the Sun, with 120% of the Sun's radius and 122% of the solar mass; as such, it shines nearly twice as brightly as the Sun. HD 219623 is around 1.2 billion years in age, [6] with a projected rotational velocity of 5.5 km/s. [8] Compared to the Sun, it has a slightly higher abundance of elements other than hydrogen and helium—what astronomers term the star's metallicity. [7] The effective temperature of the stellar atmosphere is about 6,138 K, [7] giving it the yellow-white hued glow of an ordinary F-type star. [12]

In 2006, this star was examined using the MIPS instrument on the Spitzer Space Telescope. An infrared excess at a wavelength of 70 μm was detected with 3-σ certainty. The data suggests the presence of circumstellar disk of orbiting dust, [13] which is likely being replenished via debris from comets or asteroids. The temperature of this dust indicates the inner edge of the disk annulus comes to within 0.4  AU of the host star, while the outer edge extends out to around 22 AU. [14]

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<span class="mw-page-title-main">Chi Ceti</span> Double star in the constellation Cetus

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<span class="mw-page-title-main">49 Ceti</span> Star in the constellation Cetus

49 Ceti is a single star in the equatorial constellation of Cetus. It is visible to the naked eye as a dim, white-hued star with an apparent visual magnitude of 5.607. The star is located 186 light-years away from the Solar System, based on its parallax, and is drifting further away with a radial velocity of +10 km/s. 49 Ceti has been identified as a member of the 40-million-year-old Argus Association.

Gliese 251, also known as HIP 33226 or HD 265866, is a star located about 18 light years away from the Solar System. Located in the constellation of Gemini, it is the nearest star in this constellation. It is located near the boundary with Auriga, 49 arcminutes away from the bright star Theta Geminorum; due to its apparent magnitude of +9.89 it cannot be observed with the naked eye. The closest star to Gliese 251 is QY Aurigae, which is located 3.5 light years away.

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<span class="mw-page-title-main">32 Tauri</span> Yellow-white hued subgiant star in the constellation Taurus.

32 Tauri is the Flamsteed designation for a solitary star in the zodiac constellation of Taurus. It has a visual magnitude of 5.64, making it visible to the naked eye from suburban skies. The position of this star near the ecliptic plane means that it is subject to occultations by the Moon. Parallax measurements put it at a distance of 144 light years from the Sun. It is drifting further away with a radial velocity of +31.9 km/s, having come to within 88.9 light-years some 759,000 years ago.

HD 126053 is the Henry Draper Catalogue designation for a star in the equatorial constellation of Virgo. It has an apparent magnitude of 6.25, which means it is faintly visible to the naked eye. According to the Bortle scale, it requires dark suburban or rural skies to view. Parallax measurements made by the Hipparcos spacecraft provide an estimated distance of 57 light years to this star. It is drifting closer with a heliocentric radial velocity of −19.2 km/s.

<span class="mw-page-title-main">9 Ceti</span> Star in the constellation Cetus

9 Ceti is a star in the equatorial constellation of Cetus. It has the variable star designation BE Ceti, while 9 Ceti is the Flamsteed designation. It has an apparent visual magnitude of 6.4, which is below the limit that can be seen with the naked eye by a typical observer. Based upon parallax measurements, this star is 69.6 light years away from the Sun.

HD 133002 is a possible binary star in the northern constellation of Ursa Minor. With an apparent visual magnitude of 5.65, it is faintly visible to the naked eye. The high declination of +82.5° means it is hidden from view from most of the southern hemisphere. Parallax measurements yield an estimated distance of around 142 light years from the Sun. If it was instead positioned at a distance of 33 ly (10 pc), this would be a second magnitude star. The system is drifting closer with a heliocentric radial velocity of −44 km/s.

HD 195564 is the Henry Draper Catalogue designation for a star in the southern constellation of Capricornus. It is faintly visible to the naked eye with an apparent visual magnitude of 5.65. Parallax measurements give us an estimate of its distance as 81 light years. This is a candidate wide binary system as a faint companion star shares a common proper motion with the brighter primary component.

HD 76653 is a single star in the southern constellation Vela. It is faintly visible to the naked eye with an apparent visual magnitude of +5.71. Based upon an annual parallax shift of 41.08 mas as seen from Earth, it is located 79 light years from the Sun. The star is moving closer to the Sun with a radial velocity of −6 km/s. It is a probable co-moving companion of the nearby Delta Velorum; the two have an estimated physical separation of 2.2 ly (0.6605 pc) with similar proper motions. Both are likely members of the Ursa Major association.

HD 46815 is a solitary star in the southern constellation Columba. It is faintly visible to the naked eye with an apparent magnitude of 5.4 and is estimated to be 408 light years away. However, it is receding with a heliocentric radial velocity of 32.2 km/s.

References

  1. 1 2 3 4 5 6 Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics . 649: A1. arXiv: 2012.01533 . Bibcode:2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657 . S2CID   227254300. (Erratum:  doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  2. 1 2 3 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv: 1108.4971 , Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID   119257644.
  3. 1 2 Frasca, A.; et al. (December 2009), "REM near-IR and optical photometric monitoring of pre-main sequence stars in Orion. Rotation periods and starspot parameters", Astronomy and Astrophysics, 508 (3): 1313–1330, arXiv: 0911.0760 , Bibcode:2009A&A...508.1313F, doi:10.1051/0004-6361/200913327, S2CID   118361131.
  4. 1 2 Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data, SIMBAD, Bibcode:1986EgUBV........0M.
  5. ↑ Nordström, B.; et al. (May 2004), "The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of ˜14,000 F and G dwarfs", Astronomy and Astrophysics, 418: 989–1019, arXiv: astro-ph/0405198 , Bibcode:2004A&A...418..989N, doi:10.1051/0004-6361:20035959, S2CID   11027621.
  6. 1 2 3 4 5 Boyajian, Tabetha S.; et al. (July 2013), "Stellar Diameters and Temperatures. III. Main-sequence A, F, G, and K Stars: Additional High-precision Measurements and Empirical Relations", The Astrophysical Journal, 771 (1): 31, arXiv: 1306.2974 , Bibcode:2013ApJ...771...40B, doi:10.1088/0004-637X/771/1/40, S2CID   14911430, 40. See Table 3.
  7. 1 2 3 4 5 Prugniel, P.; et al. (2011), "The atmospheric parameters and spectral interpolator for the MILES stars", Astronomy & Astrophysics, 531: A165, arXiv: 1104.4952 , Bibcode:2011A&A...531A.165P, doi:10.1051/0004-6361/201116769, S2CID   54940439.
  8. 1 2 Mishenina, T. V.; et al. (November 2012), "Activity and the Li abundances in the FGK dwarfs", Astronomy & Astrophysics, 547: 8, arXiv: 1210.6843 , Bibcode:2012A&A...547A.106M, doi:10.1051/0004-6361/201118412, S2CID   119287319, A106.
  9. ↑ "HD 219623", SIMBAD , Centre de données astronomiques de Strasbourg , retrieved 2016-03-22.
  10. ↑ Helmut A., Abt; Willmarth, Daryl (2006), "The Secondaries of Solar-Type Primaries. I. The Radial Velocities", The Astrophysical Journal Supplement Series, 162 (1): 207–226, Bibcode:2006ApJS..162..207A, doi: 10.1086/498095 , S2CID   123629445.
  11. ↑ Lépine, Sébastien; Shara, Michael M. (March 2005), "A Catalog of Northern Stars with Annual Proper Motions Larger than 0.15" (LSPM-NORTH Catalog)", The Astronomical Journal, 129 (3): 1483–1522, arXiv: astro-ph/0412070 , Bibcode:2005AJ....129.1483L, doi:10.1086/427854, S2CID   2603568.
  12. ↑ "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on March 18, 2012, retrieved 2012-01-16.
  13. ↑ Beichman, C. A.; et al. (December 2006), "New Debris Disks around Nearby Main-Sequence Stars: Impact on the Direct Detection of Planets", The Astrophysical Journal, 652 (2): 1674–1693, arXiv: astro-ph/0611682 , Bibcode:2006ApJ...652.1674B, doi:10.1086/508449, S2CID   14207148.
  14. ↑ Lawler, S. M.; et al. (November 2009), "Explorations Beyond the Snow Line: Spitzer/IRS Spectra of Debris Disks Around Solar-type Stars", The Astrophysical Journal, 705 (1): 89–111, arXiv: 0909.0058 , Bibcode:2009ApJ...705...89L, doi:10.1088/0004-637X/705/1/89, S2CID   1272803.
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