10 Cassiopeiae

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10 Cassiopeiae
Cassiopeia constellation map.svg
Red circle.svg
Location of 10 Cassiopeiae (circled)
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Cassiopeia
Right ascension 00h 06m 26.5374s [1]
Declination +64° 11′ 46.169″ [1]
Apparent magnitude  (V)5.54 - 5.59 [2]
Characteristics
Spectral type B9IIIe [2]
U−B color index −0.19 [3]
B−V color index −0.03 [3]
Variable type suspected Be [2]
Astrometry
Radial velocity (Rv)−0.61±0.54 [1]  km/s
Proper motion (μ)RA: +9.248 [1]   mas/yr
Dec.: +0.828 [1]   mas/yr
Parallax (π)3.4070 ± 0.0536  mas [1]
Distance 960 ± 20  ly
(294 ± 5  pc)
Absolute magnitude  (MV)−1.863 [4]
Details
Mass 3.2 [5]   M☉
Radius 8.3 [6]   R☉
Luminosity 920 [7]   L☉
Surface gravity (log g)2.08 [5]   cgs
Temperature 11,351 [7]   K
Metallicity [Fe/H]−0.01 [4]   dex
Rotation 1.07  d [8]
Rotational velocity (v sin i)125 [7]  km/s
Age 218 [9]   Myr
Other designations
10  Cas, HR  7, HD  144, BD+63°2107, HIP  531, NSV  15021
Database references
SIMBAD data

10 Cassiopeiae (10 Cas) is a blue-white giant star in the constellation Cassiopeia, about 960 light years away.

10 Cassiopeiae is a B9 giant star. It shows emission lines in its spectrum and is classified as a Be star. It shows slight variations in its brightness, between magnitudes 5.54 and 5.59.

At an age of 218 million years, 10 Cassiopeiae has expanded away from the main sequence after exhausting its core hydrogen and now has a radius about eight times that of the Sun. With an effective temperature of about 11,000  K , it emits nearly a thousand times the luminosity of the Sun.

Related Research Articles

1 Cancri is a single star in the zodiac constellation of Cancer, positioned near the border with Gemini at a distance of around 467 light years from the Sun. It is barely visible to the naked eye as a dim, orange-hued star with an apparent visual magnitude of 5.97. The object is moving further from the Earth with a heliocentric radial velocity of +14 km/s.

<span class="mw-page-title-main">Omega Cassiopeiae</span> Binary star system in constellation Cassiopeia

Omega Cassiopeiae is a binary star system in the northern constellation of Cassiopeia. It has a combined apparent visual magnitude of +4.99, which means it is a faint star but visible to the naked eye. Based upon an annual parallax shift of 4.65 mas as seen from Earth, this system is located roughly 730 light years from the Sun. At that distance, the visual magnitude is diminished by an extinction of 0.16 due to interstellar dust.

HD 173791 is a solitary yellow hued star located in the southern constellation Telescopium. It has an apparent magnitude of 5.80, allowing it to be viewed with the naked eye under suitable viewing conditions. Parallax measurements place the object at a distance of 364 light years, and it is currently receding from the Solar System with a heliocentric radial velocity of 9.7 km/s.

<span class="mw-page-title-main">TZ Cassiopeiae</span> Star in the constellation Cassiopeia

TZ Cassiopeaie(TZ Cas, HIP 117763, SAO 20912) is a variable star in the constellation Cassiopeia with an apparent magnitude of around +9 to +10. It is approximately 8,400 light-years away from Earth. The star is a red supergiant star with a spectral type of M3 and a temperature below 4,000 K.

29 Camelopardalis is a double star in the circumpolar constellation Camelopardalis. With an apparent magnitude of 6.59, it's right below the max visibility to the naked eye, and can only be viewed under phenomenal conditions. The star is located 484 light years away based on parallax, but is drifting further away with a radial velocity of 3.9 km/s.

<span class="mw-page-title-main">83 Ursae Majoris</span> Candidate binary star system in the constellation Ursa Major

83 Ursae Majoris is a candidate binary star system in the northern circumpolar constellation of Ursa Major. It is a semiregular variable star, and it has been given the variable star designation IQ Ursae Majoris. It ranges in brightness from apparent visual magnitude 4.69 to 4.75. Percy and Au (1994) identified it as a small amplitude red variable with an irregular behavior, having a characteristic time scale of 20 days. Based upon an annual parallax shift of 6.23±0.22 mas, it is located roughly 520 light years from the Sun. The distance derived from its Gaia Early Data Release 3 parallax is 179 pc. The system is moving closer with a heliocentric radial velocity of −18.6 km/s.

<span class="mw-page-title-main">Beta Microscopii</span> Constellation Microscopium star

Beta Microscopii, Latinized from β Microscopii, is a solitary star in the constellation Microscopium. It is close to the lower limit of stars that are visible to the naked eye having an apparent visual magnitude of 6.05 Based upon an annual parallax shift of 6.5022 mas as seen from Earth, this star is located 502 light years away from the Sun. At that distance, the visual magnitude is diminished by an extinction factor of 0.19 due to interstellar dust.

HD 167257 is a solitary star in the southern constellation Telescopium. It has an apparent magnitude of 6.05, making it faintly visible to the naked eye. Parallax measurements place the star at a distance of 420 light years and has a radial velocity of −5.1 km/s, which is poorly constrained. This indicates that it is drifting towards the Solar System.

<span class="mw-page-title-main">MZ Puppis</span> Red supergiant star in the constellation of Puppis

MZ Puppis is a red supergiant star in the constellation of Puppis. It has a radius of 400 R☉.

HD 64484 is a solitary star in the southern circumpolar constellation Volans. With an apparent magnitude of 5.76, it is faintly visible to the naked eye under dark skies. Parallax measurements place it at a distance of 458 light years but is receding with a heliocentric radial velocity of 11 km/s.

1 Trianguli is a solitary star located in the northern constellation Triangulum. With an apparent magnitude of 7.52, it is too faint to be seen with the naked eye but can be seen easily with binoculars. The star is currently 730 light years away based on parallax but is drifting away with a radial velocity of 7 km/s.

<span class="mw-page-title-main">Y Tauri</span> Variable star in the constellation Scutum

Y Tauri is a carbon star located in the constellation Taurus. Parallax measurements by Gaia put it at a distance of approximately 2,170 light-years.

Mu1 Octantis, Latinized from μ1 Octantis, is a solitary star in the southern circumpolar constellation Octans. It has an apparent magnitude of 5.98, allowing it to be faintly visible to the naked eye under ideal conditions. Located 335 light years away, it is approaching the Sun with a heliocentric radial velocity of −36 km/s.

<span class="mw-page-title-main">10 Trianguli</span> Star in the constellation Triangulum

10 Trianguli is a solitary star located in the northern constellation Triangulum. It has an apparent magnitude of 5.28, making it faintly visible to the naked eye under ideal conditions. The star is situated 363 light years away and is thought to be moving further away with a heliocentric radial velocity of 0.457 km/s, although this value varies widely depending on the study.

<span class="mw-page-title-main">Tau Octantis</span> Star in the southern constellation of Octans

Tau Octantis, Latinized from τ Octantis, is a solitary star in the southern circumpolar constellation Octans. It has an apparent magnitude of 5.50, allowing it to be faintly seen with the naked eye. The object is located at a distance of 480 light years but is receding with a heliocentric radial velocity of 31 km/s.

7 Tauri is a multiple star in the northern constellation of Taurus. It has a combined apparent visual magnitude of 5.95, so, according to the Bortle scale, it is faintly visible from suburban skies at night. Measurements made with the Gaia spacecraft show an annual parallax shift of 5.5 mas, which is equivalent to a distance of around 593 light years from the Sun.

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.

HD 191220, also known as HR 7698, is a solitary white hued star located in the southern circumpolar constellation Octans. It has an apparent magnitude of 6.14, placing it near the limit for naked eye visibility. The object is located relatively close at a distance of 245 light years based on Gaia DR3 parallax measurements but is slowly receding with a heliocentric radial velocity of 0.1 km/s. At its current distance, HD 191220's brightness is diminished by 0.22 magnitudes due to interstellar dust.

HD 59640 is a solitary white hued star located in the southern circumpolar constellation Volans. It has an apparent magnitude of 6.48, placing it near the limit for naked eye visibility. Gaia DR3 parallax measurements place the object at a distance of 262 light years and it is receding with a heliocentric radial velocity of 18.4 km/s. At its current distance, HD 59640's brightness is diminished by three tenths of a magnitude due to interstellar dust.

<span class="mw-page-title-main">2 Cassiopeiae</span> Star in the constellation Cassiopeia

2 Cassiopeiae is a white bright giant in the constellation Cassiopeia, about 2,800 light years away. It is a chemically peculiar Am star.

References

  1. 1 2 3 4 5 6 Vallenari, A.; et al. (Gaia Collaboration) (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics . arXiv: 2208.00211 . doi: 10.1051/0004-6361/202243940 . Gaia DR3 record for this source at VizieR.
  2. 1 2 3 Samus, N. N.; et al. (2017). "General Catalogue of Variable Stars". Astronomy Reports . 5.1. 61 (1): 80–88. Bibcode:2017ARep...61...80S. doi:10.1134/S1063772917010085. S2CID   125853869.
  3. 1 2 Hoffleit, D.; Jaschek, C., eds. (1991). The Bright Star Catalogue. New Haven: Yale University Observatory. Bibcode:1991bsc..book.....H.
  4. 1 2 Katz, D.; Soubiran, C.; Cayrel, R.; Barbuy, B.; Friel, E.; Bienaymé, O.; Perrin, M. -N. (2011). "Probing the Galactic thick disc vertical properties and interfaces". Astronomy and Astrophysics. 525: A90. Bibcode:2011A&A...525A..90K. doi: 10.1051/0004-6361/201014840 .
  5. 1 2 Anders, F.; Khalatyan, A.; Chiappini, C.; Queiroz, A. B.; Santiago, B. X.; Jordi, C.; Girardi, L.; Brown, A. G. A.; Matijevič, G.; Monari, G.; Cantat-Gaudin, T.; Weiler, M.; Khan, S.; Miglio, A.; Carrillo, I.; Romero-Gómez, M.; Minchev, I.; De Jong, R. S.; Antoja, T.; Ramos, P.; Steinmetz, M.; Enke, H. (2019). "Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia DR2 stars brighter than G = 18". Astronomy and Astrophysics. 628: A94. arXiv: 1904.11302 . Bibcode:2019A&A...628A..94A. doi:10.1051/0004-6361/201935765. S2CID   131780028.
  6. ↑ Stassun, Keivan G.; et al. (2019-10-01). "The Revised TESS Input Catalog and Candidate Target List". The Astronomical Journal. 158 (4): 138. arXiv: 1905.10694 . Bibcode:2019AJ....158..138S. doi:10.3847/1538-3881/ab3467. hdl: 1721.1/124721 . ISSN   0004-6256. S2CID   166227927.
  7. 1 2 3 Zorec, J.; Frémat, Y.; Domiciano De Souza, A.; Royer, F.; Cidale, L.; Hubert, A.-M.; Semaan, T.; Martayan, C.; Cochetti, Y. R.; Arias, M. L.; Aidelman, Y.; Stee, P. (2017). "Critical study of the distribution of rotational velocities of Be stars". Astronomy & Astrophysics. 595: A132. arXiv: 1702.07684 . Bibcode:2016A&A...595A.132Z. doi:10.1051/0004-6361/201628760.
  8. ↑ Oelkers, Ryan J.; Rodriguez, Joseph E.; Stassun, Keivan G.; Pepper, Joshua; Somers, Garrett; Kafka, Stella; Stevens, Daniel J.; Beatty, Thomas G.; Siverd, Robert J.; Lund, Michael B.; Kuhn, Rudolf B.; James, David; Gaudi, B. Scott (2018). "Variability Properties of Four Million Sources in the TESS Input Catalog Observed with the Kilodegree Extremely Little Telescope Survey". The Astronomical Journal. 155 (1): 39. arXiv: 1711.03608 . Bibcode:2018AJ....155...39O. doi:10.3847/1538-3881/aa9bf4. S2CID   119515775.
  9. ↑ Gontcharov, G. A. (December 2012). "Dependence of kinematics on the age of stars in the solar neighborhood". Astronomy Letters. 38 (12): 771–782. arXiv: 1606.08814 . Bibcode:2012AstL...38..771G. doi:10.1134/S1063773712120031. ISSN   0320-0108. S2CID   118345778.
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