Mu Herculis

Ficha d'oxetu celesteMu Herculis
Estrella múltiple
Datos d'observación
Ascensión reuta (α) 266,614625 °[1]
Declinación (δ) 27,720639 °[1]
Constelación Hércules (es) Traducir[2]
Otros nomes
Cambiar los datos en Wikidata

Coordenaes: Sky map 17h 46m 27.51s, 27° 43′ 14.3″

Mu Herculis (μ Her / 86 Herculis) ye un sistema estelar na constelación d'Hércules de magnitú aparente +3,42. Anque nun tien nome propiu habitual, na astronomía china yera conocida como Kew Ho, «Los Nueve Ríos».[3] Alcuéntrase a namái 27,4 años lluz del Sistema Solar. La estrella conocida más cercana a esti sistema ye Gliese 686, distante 4,5 años lluz, ente que la brillosa Vega (α Lyrae), alcuéntrase a 7,3 años lluz d'ella.[4]

Mu Herculis ye una sistema triple o cuádruplu, que la so estrella principal, Mu Herculis A (LHS 3326 / GJ 695 A),[5] ye una subxigante mariella de tipu espectral G5IV con una temperatura efectivo d'aproximao 5500 K. Hasta apocayá taba na secuencia principal pero ta empezando a crecer, evolucionando escontra una xigante colorada. De masa poco mayor que'l Sol, la so lluminosidá ye 2,7 vegaes mayor que la lluminosidá solar —considerando la radiación infrarroxo emitida— y el so radiu equival a 1,76 radios solares. Xira sobre sigo mesma siquier 10 vegaes más apriesa que'l Sol, con un periodu de rotación inferior a 4,3 díes. De resultes d'ello amuesa actividá magnética y ye una fonte emisora de rayos X.[6] El so conteníu metálico ye cimeru a la solar, siendo'l so índiz de metalicidá [Fe/H] = +0,20.[7]

Otros dos componentes del sistema formen una binaria que la so separación al respective de Mu Herculis A ye de siquier 300 UA.[6] Felicidad binaria emplega unos 3445 años en completar una órbita en redol a la subxigante mariella.[8] Mu Herculis B (LHS 3325 / GJ 695 B)[9] ye una fría nana colorada de tipu espectral M3.5V. La so temperatura efectivo ye de 3300 K y la so lluminosidá bolométrica apenes supón el 5% de la del Sol.[10] Mu Herculis C (GJ 695 C)[11] tamién ye una nana colorada daqué más pequeña y menos lluminosa que la componente B. La separación media ente les componentes B y C ye de 2,2 UA —anque la escentricidá de la órbita fai qu'ésta varie ente 1,5 y 3,6 UA—, siendo el so periodu orbital de 43 años.[6]

Piénsase que, amás, Mu Herculis A tien una compañera invisible bien próxima a ella. Denominada Mu Herculis Ab, puede tener un quintu de la masa solar, completando una órbita en redol a Mu Herculis A cada 64 años.[8]

Ver tamién

Referencies

  1. ↑ 1,0 1,1 «The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog» (n'inglés). The Astronomical Journal (6):  páxs. 3466–3471. avientu 2001. doi:10.1086/323920. 
  2. ↑ Afirmao en: VizieR. Llingua de la obra o nome: inglés.
  3. ↑ Allen, Richard Hinckley (1889). «Hercules», Courier Dover Publications: Star Names — Their Lore and Meaning (n'inglés), páx. 563. ISBN 0-486-21079-0. Consultáu'l 24 de marzu de 2012.
  4. ↑ Mu Herculis (Solstation)
  5. ↑ Mu Herculis A (SIMBAD)
  6. ↑ 6,0 6,1 6,2 Mu Herculis (Stars, Jim Kaler)
  7. ↑ Soubiran, C.; Bienaymé, O.; Mishenina, T. V.; Kovtyukh, V. V. (2008). «Vertical distribution of Galactic disk stars. IV. AMR and AVR from clump giants». Astronomy and Astrophysics 480 (1). páxs. 91-101. http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?2008A%26A...480...91S&db_key=AST&nosetcookie=1. 
  8. ↑ 8,0 8,1 Tokovinin, A. (2008). «Comparative statistics and origin of triple and quadruple stars». Monthly Notices of the Royal Astronomical Society 389 (2). páxs. 925-938. http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?2008MNRAS.389..925T&db_key=AST&nosetcookie=1. 
  9. ↑ Mu Herculis B (SIMBAD)
  10. ↑ Morales, J. C.; Ribas, I.; Jordi, C. (2008). «The effect of activity on stellar temperatures and radii». Astronomy and Astrophysics 478 (2). páxs. 507-512. http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?2008A%26A...478..507M&db_key=AST&nosetcookie=1. 
  11. ↑ Mu Herculis C (SIMBAD)

Coordenaes: Sky map 17h 46m 27.51s, 27° 43′ 14.3″

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