Edge Rewrite
everything Source code View original
// HTMLRewriter · presentation

This page was redesigned at the edge.

Cloudflare fetched the original article and streamed it through HTMLRewriter to apply an entirely new visual system without rebuilding the source page.

// request.cf · coarse context

A page that knows where it met you.

Only coarse request metadata is shown. This demo does not display or persist visitor IP addresses.

Country
US
Cloudflare location
CMH
Connection
HTTP/2
Language
Not provided

Ray ID: a241fdc27c0fa8fe

Jump to content

// Workers AI · dad joke modeWhat did 10 Cassiopeiae say to its friend? You're a star.

From Wikipedia, the free encyclopedia
(Redirected from MWC 2)
10 Cassiopeiae
Location of 10 Cassiopeiae (circled)
Observation data
Epoch J2000.0      Equinox ICRS
Constellation Cassiopeia[1]
Right ascension 00h 06m 26.5374s[2]
Declination +64° 11′ 46.169″[2]
Apparent magnitude (V) 5.54 - 5.59[3]
Characteristics
Spectral type B9IIIe[3]
U−B color index −0.19[4]
B−V color index −0.03[4]
Variable type suspected Be[3]
Astrometry
Radial velocity (Rv)−0.61±0.54[2] km/s
Proper motion (μ) RA: +9.248[2] mas/yr
Dec.: +0.828[2] mas/yr
Parallax (π)3.4070±0.0536 mas[2]
Distance960 ± 20 ly
(294 ± 5 pc)
Absolute magnitude (MV)−1.863[5]
Details
Mass3.2[6] M☉
Radius8.3[7] R☉
Luminosity920[8] L☉
Surface gravity (log g)2.08[6] cgs
Temperature11,351[8] K
Metallicity [Fe/H]−0.01[5] dex
Rotation1.07 d[9]
Rotational velocity (v sin i)125[8] km/s
Age218[10] Myr
Other designations
10 Cas, HR 7, HD 144, BD+63°2107, HIP 531, NSV 15021, MWC 2
Database references
SIMBADdata

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.

References

[edit]
  1. ↑ Anderson, E.; Francis, Ch. (May 2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331–346. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. eISSN 1562-6873. ISSN 1063-7737. S2CID 119257644.
  2. 1 2 3 4 5 6 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  3. 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.
  4. 1 2 Hoffleit, D.; Jaschek, C., eds. (1991). The Bright Star Catalogue. New Haven: Yale University Observatory. Bibcode:1991bsc..book.....H.
  5. 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.
  6. 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.
  7. ↑ 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.
  8. 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.
  9. ↑ 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.
  10. ↑ 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.
Retrieved from "https://en.wikipedia.org/w/index.php?title=10_Cassiopeiae&oldid=1329902759"