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Tipo Espectral UNIVERSIDAD COMPLUTENSE DE MADRID FACULTAD DE CIENCIAS FÍSICAS Departamento de Física de la Tierra, Astronomía y Astrofísica II TESIS DOCTORAL Estudio de la actividad cromosférica en sistemas binarios MEMORIA PARA OPTAR AL GRADO DE DOCTOR PRESENTADA POR David Montes Gutiérrez Directora María José Fernández Figueroa Madrid, 2015 © David Montes Gutiérrez, 1995 1 UNIVERSIDAD COMPLUTENSE DE MADRID FACULTAD DE CIENCIAS FíSICAS Departamento de Física de La. Tierra Astronomía y Astrofísica JI (ASTROFíSICA Y CIENCIAS DE LA ATMOSFERA) *““‘u””.5309545438* UNIVERSIDAD COM~LUTENSE ESTUDIO DE LA ACTIVIDAD CROMOSFERICA EN SISTEMAS BINARIOS Dirigido lor: Dra. María José Fernández Figueroa Memoria 1)rese1~tada por Da;id Montes Gutiérrez para aspirar al grado de DOCTOR en Ciencias Físicas Madrid, Diciembre 1994 1 Agradecimientos El presente trabajo ha sido realizado bajo la dirección de la Dra. María José Fernández Figueroa, a quien deseo expresar mi mas sincero agradecimiento por su valiosa y constante ayuda. Por otro lado también deseo hacer patente mi agradecimiento: Al director del Departamento Prof. Manuel Rego. A todos los miembros del grupo de actividad estelar del Departamento: Prof. Elisa De Castro, Prof. Manuel Comide y los doctorandos Fernando Martín, Rosario Lorente y David Barrado. A Javier Armentia por su participación en la realización y reducción de algunas de las observaciones iniciales utilizadas en este trabajo. Al Dr. Benjamin Montesinos por su valiosos consejos y sugerencias. A todos los demas miembros del Departamento: Prof. Jaime Zamorano, Prof. Javier Gorgas, Dr. Luis F. Miranda y los doctorandos Jesus Gallego, Alvaro Vitores, Marta Cordero, Nicolas Cardiel, E. de Borja Domínguez, Almudena Alonso, Oscar Alonso y Santos Pedraz, por su importante ayuda y constante estímulo. A el personal del Observatorio de Calar Alto (Almería) y del Observatorio del Roque de Los Muchachos (La Palma) por su ayuda durante la realización de las observaciones. A la Universidad Complutense de Madrid, gracias a la cual disfruto de una plaza de Profesor Ayudante E.U. que me ha permitido seguir adelante, durante todo este tiempo, en la realización de este trabajo. 11 Indice 1 Introducción 1 1.1 Actividad estelar 1 1.2 Indicadores de actividad estelar 3 1.3 Estrellas especialmente activas 4 1.3.1 Sistemas binarios RS CVn 5 1.3.2 Estrellas BY Dra 7 1.3.3 Diferentes estructuras activas 7 1.4 Resumen del trabajo 9 2 Observaciones y reducción 11 2.1 Observaciones 11 2.2 Estrellas observadas • . 12 2.2.1 Sistemas binarios cromosféricamente activos • . 13 2.2.2 Estrellas aisladas o componentes de sistemas binarios visuales 14 2.3 Reducción de las observaciones 19 2.3.1 Lectura de los datos 19 2.3.2 Eliminación de columnas irrelevantes 19 2.3.3 Substracción del Dark 19 2.3.4 Corrección de Fiat-Fieh! 20 2.3.5 Extracción del espectro • . 20 2.3.6 Calibración en longitud de Onda 21 2.3.7 Corrección de extinción atmosférica 22 2.3.8 Calibración en flujo absoluto . 22 2.3.9 Normalización del espectro 23 3ta línea Ha 25 3.1 Introducción 25 3.2 La línea Ha en estrellas no activas 26 3.2.1 Las estrellas de referencia 27 3.2.2 Identificación de las lineas 28 iii iv INDICE 3.3 Exceso de emisión Ha 28 3.4 Determinación de la EW de emisión 30 3.4.1 Método BDM 30 3.4.2 Técnica de Substracción Espectral 32 3.4.3 Otros índices de actividad Ha 36 3.4.4 Obtención del flujo superficial en Ha 39 3.5 Exceso de emisión Hfl 40 3.6 Resumen 42 4 Las líneas H y 1< de Ca II 45 4.1 Introduccion 45 4.2 Parámetros característicos de las lineas H y K de Ca II 46 4.2.1 Anchuras 47 4.2.2 Asimetrías 47 4.2.3 El cociente K/H 48 4.3 Los primeros índices de actividad en H y K de Ca u 50 4.3.1 Estimación visual de la intensidad 50 4.3.2 El índice fotométrico 5 51 4.4 Substracción de la contribución fotosférica 52 4.4.1 Substracción de un flujo mínimo 52 4.4.2 Substracción del flujo fotosférico teórico 52 4.4.3 Reconstrucción del perfil de absorción de la línea 54 4.4.4 Substracción espectral 55 4.4.5 Método utilizado 56 4.5 Conversión a flujo superficial 56 4.5.1 Factor Conversión, O 56 4.5.2 Relación entre F(A2) y un índice de color . 58 4.5.3 Seudo-continuo en 3950.5 Á 59 4.5.4 Flujo absoluto en las alas de la línea 59 4.5.5 Método utilizado 60 4.6 Unidades apropiadas para el nivel de actividad en II y K de Ca II 61 4.6.1 RIiK 61 4.6.2 APi jx 61 4.6.3 Aíu= 61 4.6.4 W~ 62 4.6.5 0(K) 62 4.7 Resumen 63 5 La relación de Wilson-Bappu 73 iNDICE y 73 5.1 Introducción 74 5.2 La muestra de estrellas 75 5.2.1 Magnitudes visuales absolutas, Mv 77 5.2.2 Parámetros medidos en las lineas U y K de Ca u 77 5.3 La relación de Wilson-Bappu 77 5.3.1 Definición de W 81 5.3.2 Comparacion con otras medidas de W 0(K) 82 5.3.3 Relaciones (log W0(K), Mv) propuestas 83 5.4 ¿Qué parámetros afectan a la relación de Wilson-Bappu? 83 5.4.1 El efecto de la intensidad 85 5.4.2 Influencia del ensanchamiento rotacional 87 5.5 Relación anchura-luminosidad para W~ 90 5.6 Relaciones entre anchuras e intensidades 91 5.6.1 Relación entre W1(K) y I~3 94 5.6.2 Relación entre W1(K) y W0(K) 95 5.6.3 El cociente K/H 96 5.7 Relación anchura luminosidad para la linea He 97 5.8 Resumen 99 6 Análisis de los sistemas observados 99 6.1 Grupo 1 99 6.1.1 13 Cet (A) (UD 3196, UR 142) 101 6.1.2 UV Psc (liD 7700) 102 6.1.3 VY Arí (lID 17433) 104 6.1.4 V833 Tau (UD 283750, G1171.2 A) . 104 6.1.5 OU Gem (HD 45088) • . 107 6.1.6 SV Cam (UD 44982) 107 6.1.7 YY Gem (Castor C, BD +32 1582, GL 278 O) • . 108 6.1.8 BF Lyn (UD 80715) 110 6.1.9 Dli Leo (MD 86590) 112 6.1.10 ~ UMa (B) (53 UMa, UD 98230, HR 4374) 113 6.1.11 AS Dra (UD 107760) 115 6.1.12 IL Com (UD 108102) 117 6.1.13 MD 131511 (MR 5553) 117 6.1.14 MS Ser (UD 143313) 2 CrB (17 CrB, TZ CrB, lID 146361, UR 6063) 118 6.1.15 a V772 Her (HD 165590, ADS 1 1O6OAB) 121 6.1.16 V815 Her (UD 166181) . 121 6.1.17 6.1.18 BY Dra (UDE 234677) 123 vi INDICE 6.1.19 V775 Her (UD 175742) 125 6.1.20 V478 Lyr (HD 178450) 128 6.1.2 1 ER Viii (liD 200391) 128 6.1.22 KZ And (B) (liD 218738) 130 6.1.23 Kl Peg (HD 222317) 133 6.2 Grupo 2 134 6.2.1 AR Psc (liD 8357) 134 6.2.2 LX Per (BD +47 781) 137 6.2.3 UX Ari (UD 21242) 137 6.2.4 Y711 Tau (BR 1099, MD 22468) 139 6.2.5 El En (liD 26337) 143 6.2.6 VV Mon (BD -05 1935) 143 6.2.7 54 Cam (AE Lyn, HD 65626, HR 31 19) 145 6.2.8 RU Cnc (BD +24 1959) 147 6.2.9 TY Pyx (UD 77137) 147 6.2.10 RW UMa (BD +52 1579) 148 6.2.11 HU Vir (liD 106225) 150 6.2.12 UX Com (UD +29 2355) 151 6.2.13 HD 113816 (BD-04 3419) 151 6.2.14 RS CVn (UD 114519) 52 6.2.15 BH CVn (UD 118216, HR 5110) 153 6.2.16 Uy Lib (lID 128171) 154 6.2.17 SS Boo (BD +39 2849) 154 6.2.18 Rl CrB (HD 139588) 154 6.2.19 WW Dra (UD 150708) 156 6.2.20 HR 6469 (V819 Her, HD 157482) 158 6.2.21 Z Her (HD 163930) 159 6.2.22 MM Her (HD 341475) 161 6.2.23 AW Her (UD 348635) 163 6.2.24 42 Cap (HD 206301, HR 8283) 165 6.2.25 Rl Lac (MD 209318) 166 6.2.26 AR Lac (lID 210334, BR 8448) 168 6.2.27 SZ Psc (HD 219113) 170 6.2.28 II Peg (MD 224085) 173 6.3 Grupo 3 175 6.3.1 33Psc(HD28,HR3) 175 6.3.2 5 Cet (AP Psc liD 352, HR 14) 175 6.3.3 UD Cet (liD 1833) 177 INDICE vii 177 6.3.4 ( And (34 And, liD 4502, HR 215) 178 6.3.5 i~ And (38 Aud UD 5516, UR 271) 178 6.3.6 AY Cet (39 Cet, HD 7672, UR 373) 181 6.3.7 liD 12545 (XX Tri, BD +34 363) R 642 ).. 182 6.3.8 6 lri A (IZ lri A, ¡. Tri A, UD 13480, H 182 6.3.9 RZ En (HD 30050) 183 6.3.10 12 Cam (BM Cam, UD 32357, UIt 1623) 184 6.3.11 V1149 Qn (liD 37824) 6.3.12 CQ Aur (UD 250810) 187 6.3.13 SS Cam 188 6.3.14 AR Mon (HD 57364) • .
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