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Investigación Y Ciencia CIEN AÑOS DEL DIAGRAMA DE HERTZSPRUng-RUssell LA TABLA PERIÓDICA 0 B A F G K M 10.000.000 TIPO ESPECTRAL DE LAS ESTRELLAS –12 TIPO Y COLOR ESTELAR –11 De manera parecida a lo que ocurre cuando calentamos un metal, el color de una estrella es indicativo de la temperatura de su superficie: desde un rojo tibio derecha( ) 1.000.000 –10 hasta un azul candente (izquierda). Ello permite dividir a las estrellas en siete tipos ETA CARINAE espectrales, denotados O, B, A, F, G, K y M. Estos se basan en los elementos químicos –9 que absorben luz en las capas externas, lo que a su vez depende de la temperatura. En castellano, una regla mnemotécnica para recordarlos es: «Otros Buenos DENEB Astrónomos Fueron Galileo, Kepler y Messier». –8 ) Sol 100.000 RIGEL MU CEPHEI O ( R136A1 SECUENCIA PRINCIPAL h ALPHA CAMELOPARDALIS –7 La mayoría de las estrellas se extienden a lo largo de la diagonal que cruza el ALNILAM diagrama de la parte superior izquierda a la esquina inferior derecha. Ello se debe a que tanto la luminosidad como la temperatura de la mayor parte de las estrellas BETELGEUSE –6 CANOPUS ANTARES ); ESA/NASA/SO VV CEPHEI vienen determinadas por un tercer parámetro: la masa. Las estrellas más calientes ZETA PUPPIS IOTA ORIONIS ETA LEONIS y brillantes (izquierda) poseen una masa mayor. Una vez que una estrella comienza 10.000 SAIPH –5 89 HERCULIS THETA1 ORIONIS C BETA CANIS MAJORIS PI PUPPIS a producir energía gracias a las reacciones nucleares de fusión del hidrógeno, MIRFAK ENIF BETA CENTAURI EPSILON GEMINORUM se alcanza un estado de equilibrio y el astro se mantiene en la misma posición ZETA OPHIUCHI ZETA GEMINORUM ADHARA BETA LYRAE A POLARIS LAMBDA VELORUM –4 AE AURIGAE 1 ETA AQUILAE del diagrama durante la mayor parte de su vida. de la Hélice nebulosa ALPHA CRUCIS BETA CAMELOPARDALIS BETA CRUCIS SPICA ALPHA AQUARII ZETA AURIGAE AO ( AO 2 DELTA CEPHEI BETA AQUARII S r ALPHA CRUCIS SHAULA A ALMACH –3 GIGANTES/SUPERGIGANTES MU COLUMBAE BELLATRIX ALCYONE E r, N r, ACHERNAR BETA DRACONIS Estas estrellas abandonaron la secuencia 1000 SHAULA B T ALBIREO A principal cuando agotaron el hidrógeno del Recto ATLAS N ELECTRA MIRACH MENKAR ALPHA HERCULIS –2 MEROPE A ALPHARD núcleo y comenzaron a quemar otras A. T. BETA PEGASI BETA GRUIS Y EL NATH Ci THUBAN G reservas de combustible, como el helio. Las ZUBENESCHAMALI S I DUBHE ETAMIN MU GEMINORUM más masivas se convierten en supergigantes; PLEIONE U P E R G KOCHAB –1 r, STS r, ALKAID ALHENA ALDEBARAN REGULUS BETA CORVI ALGEIBA A GAMMA CRUCIS las menores, en gigantes. Si una supergigante ne ALBIREO B DENEB KAITOS ix ALIOTH ARCTURUS E 100 0 ocupase el lugar del Sol, su tamaño abarcaría ALGOL A COR CAROLI MIZAR A DELTA SCUTI CAPELLA Ab CAPELLA Aa hasta la órbita de Júpiter. Estas estrellas no se M /M. PHECDA MERAK ALGEIBA B HAMAL GEMMA MENKALINAN RR LYRAE ETA DRACONIS mantienen fijas en el diagrama, sino que se EAM VEGA ZUBENELGENUBI Betelgeuse T POLLUX +1 RASALHAGUE BETA CASSIOPEIAE MIRA desplazan a medida que evolucionan. SIRIUS A MEGREZ G A N ALDERAMIN I T ebula FOMALHAUT G E DENEBOLA S ix N ix ALCOR +2 HIPERGIGANTES ALTAIR RS CANUM VENATICORUM hEL ETA BOÖTIS Las estrellas más masivas de todas se hallan 10 BETA PICTORIS S GAMMA DORADUS PROCYON A en la parte superior izquierda. El récord lo BETA HYDRI +3 hUBBLE E GAMMA VIRGINIS XI OPHIUCHI A posee R136a1, que nació con una masa 320 UPSILON ANDROMEDAE KAPPA FORNACIS PI3 ORIONIS veces superior a la del Sol, si bien desde C NU PHOENICIS BETA COMAE BERENICES IOTA HOROLOGII +4 entonces ha perdido parte de su material en CHI DRACONIS A MU ARAE U 16 CYGNI B forma de vientos estelares. Otra estrella muy ZETA TUCANAE ETA CASSIOPEIAE A DELTA PAVONIS YN/NOAO/ESA/ 14 HERCULIS 1 1 wi E SOL 54 PISCIUM +5 masiva e inestable es Eta Carinae, la cual se CHI ORIONIS A 61 VIRGINIS ALPHA MENSAE N ZETA2 RETICULI 82 ERIDANI 70 OPHIUCHI A halla envuelta en una nebulosa de gas como XI BOOTIS A 12 OPHIUCHI 47 URSAE MAJORIS 1 ALPHA CENTAURI B NASA/ ; ZETA RETICULI ) TAU CETI 107 PISCIUM C 16 CYGNI A 2 eta carinae resultado de una violenta eyección de SIGMA DRACONIS OMICRON ERIDANI A +6 material que ocurrió hace 170 años. I ALPHA CENTAURI A MU CASSIOPEIAE A 36 OPHIUCHI A EPSILON ERIDANI A 51 PEGASI 36 OPHIUCHI B 18 SCORPII GROOMBRIDGE 1830 Eta Carinae Eta CHI DRACONIS B P EPSILON INDI +7 ENANAS BLANCAS 36 OPHIUCHI C 1⁄10 R BY DRACONIS A 70 OPHIUCHI B Son el remanente que deja la inmensa ( /NASA 61 CYGNI A O XI BOOTIS B d I LUMINOSIDAD (UNIDADES SOLARES) (UNIDADES LUMINOSIDAD mayoría de las estrellas una vez que han A +8 LUMINOSIDAD (MAGNITUD ASOLUTA) (MAGNITUD LUMINOSIDAD r N GROOMBRIDGE 1618 61 CYGNI B agotado todo el combustible nuclear. Ya no BY DRACONIS B olo C ETA CASSIOPEIAE B LACAILLE 8760 C HZ 43 A pueden generar energía, por lo que se E GLIESE 890 YY GEMINORUM +9 comprimen por su propio peso hasta alcanzar d I A GLIESE 229 A id P un tamaño similar al de la Tierra. A pesar de S r LACAILLE 9352 E 1⁄100 +10 iv A su nombre, brillan en un amplio abanico de GROOMBRIDGE 34 A N LALANDE 21258 A LALANDE 21185 colores. Con el tiempo, se van desplazando U , WOLF 630 A SE LB 1497 L r 2 KAPTEYN’S STAR AD LEONIS nebulosa DE la HÉLICE hacia la derecha del gráfico hasta que dejan O OMICRON ERIDANI B +11 STRUVE 2398 A M SIRIUS B EQ PEGASI A de ser visibles. EV LACERTAE ON ZZ CETI GLIESE 581 KRÜGER 60 A GLIESE 876 ); J ); GD 165 G 29-38 WOLF 1061 +12 LUYTEN’S STAR STRUVE 2398 B YZ CANIS MINORIS EL SOL 1⁄1000 El Sol es una estrella de la secuencia principal. STEIN 2051 A OMICRON2 ERIDANI C Betelgeuse ( WOLF 629 +13 Nació en forma de una protoestrella fría; una EG 82 PROCYON B ROSS 154 ROSS 614 A GROOMBRIDGE 34 B BARNARD’S STAR vez que agote su hidrógeno se convertirá en ESO , EQ PEGASI B STEIN 2051 B KRÜGER 60 B ROSS 128 una gigante roja y, después, en una enana ella +14 rv YZ CETI blanca. El Sol no es tan común como suele E E VAN MAANEN’S STAR N ROSS 248 GICLAS 208–44 A afirmarse: alrededor del 95 por ciento de las K ); P. 1⁄10.000 A WOLF 424 A N LUYTEN 726–8 A +15 estrellas ocupan posiciones inferiores en el A S GICLAS 240–72 GJ 1061 GICLAS 9–38 A B L LP 658–2 LHS 288 diagrama. A LUYTEN 789–6 A GICLAS 208–45 N PROXIMA CENTAURI LUYTEN 726–8 B +16 datos estelares datos C ( A ROSS 614 B ell S WOLF 359 w os GICLAS 51-15 +17 r ENANAS MARRONES C TEEGARDEN’S STAR 1⁄100.000 LHS 292 Uno de los retos de la astrofísica actual consiste en detectar y estudiar enanas ESO 439–26 KEN VB 8 marrones, estrellas tan ligeras que no logran mantener los procesos de fusión ); LHS 3003 +18 nuclear. En el diagrama se solapan con las estrellas más débiles y rojas de la esquina gráfico ( VAN BIESBROECK’S STAR E inferior derecha (por ejemplo, LP 944-20 es una de ellas) y se extenderían más allá iv LHS 2065 +19 del diagrama en esa dirección. A fin de clasificarlas, hace una década se añadieron act DENIS 1048–3956 r TEMPERATURA SUPERFICIAL LHS 2924 los tipos espectrales L y T (no mostrados en la figura). SCR 1845–6357 A nte 1⁄1.000.000 (GRADOS KELVIN) LP 944–20 +20 h i tc i P 50.000 K 31.000 K 10.000 K 7500 K 6000 K 5300 K 3900 K 2200 K.
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