DL Crucis

DL Crucis
Dados observacionais (J2000)
Constelação Crux
Asc. reta 12h 14m 16,9s[1]
Declinação -64° 24′ 30,7″[1]
Magnitude aparente 6,238[1]
Características
Tipo espectral B1.5 Ia[1]
Cor (U-B) -0,72[1]
Cor (B-V) 0,065[1]
Variabilidade α Cygni[2]
Astrometria
Velocidade radial -10,5 km/s[1]
Mov. próprio (AR) -5,51 mas/a[3]
Mov. próprio (DEC) -0,01 mas/a[3]
Paralaxe 0,4107 ± 0,0226 mas[3]
Distância 7941 ± 437 anos-luz
2435 ± 134 pc
Magnitude absoluta -6,9[4]
Detalhes
Massa 30[5] M
Raio 42[4] R
Gravidade superficial 2,5 cgs (log g)[5]
Luminosidade 250 000[4] L
Temperatura 20 100[5] K
Rotação >43 km/s[5]
Outras denominações
DL Crucis, CD-63 732, HR 4653, HD 106343, HIP 59678, SAO 251803.[1]
DL Crucis

DL Crucis é uma estrela variável na constelação de Crux. Tem uma magnitude aparente de 6,24,[1] sendo visível a olho nu apenas em excelentes condições de visualização. É uma estrela supergigante com um tipo espectral de B1.5 Ia[1] e temperatura efetiva de 20 100 K,[5] portanto emite luz de coloração azul-branca.[6] Possui uma massa de 30 vezes a massa solar,[5] um raio de 42 raios solares e está brilhando com 250 000 vezes a luminosidade solar.[4]

A sonda astrométrica Gaia determinou para DL Crucis uma paralaxe de de 0,4107 ± 0,0226 milissegundos de arco, correspondendo a uma distância de aproximadamente 2 400 parsecs (7 900 anos-luz), com uma incerteza de 130 parsecs.[3] Esse valor é inferior ao estimado anteriormente por métodos indiretos, de 3 300 parsecs.[7]

DL Crucis é uma variável Alpha Cygni, com sua magnitude aparente variando entre 6,24 e 6,28 ao longo de um período de 2,8778 dias.[2]

Curva de luz (dados da sonda Hipparcos) de DL Crucis assumindo um período de 2,8778 dias

Ver também

Referências

  1. a b c d e f g h i j «SIMBAD query result - V* DL Cru». SIMBAD. Centre de Données astronomiques de Strasbourg. Consultado em 16 de julho de 2014 
  2. a b «VSX : Detail for DL Cru». The International Variable Star Index. American Association of Variable Star Observers (AAVSO). Consultado em 16 de julho de 2014 
  3. a b c d Gaia Collaboration: Brown, A. G. A.; Vallenari, A.; Prusti, T.; et al. (maio de 2021). «Gaia Early Data Release 3. Summary of the contents and survey properties». Astronomy & Astrophysics. 649: A1, 20 pp. Bibcode:2021A&A...649A...1G. arXiv:2012.01533Acessível livremente. doi:10.1051/0004-6361/202039657  Catálogo VizieR
  4. a b c d Lefever, K.; Puls, J.; Aerts, C (março de 2007). «Statistical properties of a sample of periodically variable B-type supergiants. Evidence for opacity-driven gravity-mode oscillations». Astronomy and Astrophysics. 463 (3). pp. 1093–1109. Bibcode:2007A&A...463.1093L. doi:10.1051/0004-6361:20066038 
  5. a b c d e f Fraser, M.; Dufton, P. L.; Hunter, I.; Ryans, R. S. I (maio de 2010). «Atmospheric parameters and rotational velocities for a sample of Galactic B-type supergiants». Monthly Notices of the Royal Astronomical Society. 404 (3). pp. 1306–1320. Bibcode:2010MNRAS.404.1306F. doi:10.1111/j.1365-2966.2010.16392.x 
  6. «The Colour of Stars», Commonwealth Scientific and Industrial Research Organisation, Australia Telescope, Outreach and Education, 21 de dezembro de 2004, consultado em 17 de julho de 2014 
  7. Jenkins, Edward B.; Tripp, Todd M (junho de 2011). «The Distribution of Thermal Pressures in the Diffuse, Cold Neutral Medium of Our Galaxy. II. An Expanded Survey of Interstellar C I Fine-structure Excitations». The Astrophysical Journal. 734 (1). pp. artigo 65, 32. Bibcode:2011ApJ...734...65J. doi:10.1088/0004-637X/734/1/65 
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