MASSIVE STARS IN THE LOCAL UNIVERSE (Q3135222): Difference between revisions
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(Created claim: summary (P836): MASSIVE STARS ARE KEY AGENTS IN THE CHEMICAL AND DYNAMIC EVOLUTION OF THE UNIVERSE. NOT ONLY DO THEY CONTINUOUSLY RELEASE RADIATIVE AND MECHANICAL ENERGY OVER MILLIONS OF YEARS TO THE SURROUNDING ENVIRONMENT ALONG WITH NEWLY FORMED ELEMENTS. THEY ALSO EXPLOIT AS SUPERNOVAE OF DIFFERENT TYPES WHEN THEY REACH THEIR FINAL MOMENT, INJECTING IN A FEW SECONDS COMPARABLE AMOUNTS OF ENERGY AND CONTAMINATING THE MEDIUM WITH HEAVY ELEMENTS. ITS IMPACT IS...) |
(Changed label, description and/or aliases in en: translated_label) |
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MASSIVE STARS IN THE LOCAL UNIVERSE | |||
Revision as of 12:30, 12 October 2021
Project Q3135222 in Spain
| Language | Label | Description | Also known as |
|---|---|---|---|
| English | MASSIVE STARS IN THE LOCAL UNIVERSE |
Project Q3135222 in Spain |
Statements
171,348.1 Euro
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201,586.0 Euro
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85.0 percent
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1 January 2016
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31 December 2019
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INSTITUTO DE ASTROFISICA DE CANARIAS (IAC)
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28°29'8.77"N, 16°18'57.38"W
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38023
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LAS ESTRELLAS MASIVAS SON AGENTES CLAVE EN LA EVOLUCION QUIMICA Y DINAMICA DEL UNIVERSO. NO SOLO LIBERAN CONTINUAMENTE DURANTE MILLONES DE AÑOS ENERGIA RADIATIVA Y MECANICA AL MEDIO QUE LAS RODEA JUNTO CON ELEMENTOS RECIENTEMENTE FORMADOS. TAMBIEN EXPLOTAN COMO SUPERNOVAS DE DIFERENTES TIPOS CUANDO ALCANZAN SU MOMENTO FINAL, INYECTANDO EN UNOS POCOS SEGUNDOS CANTIDADES COMPARABLES DE ENERGIA Y CONTAMINANDO EL MEDIO CON ELEMENTOS PESADOS. SU IMPACTO ES ENORME A PESAR DE SU PEQUEÑO NUMERO. _x000D_ NUESTRA INVESTIGACION EN ESTRELLAS MASIVAS SE CENTRARA DURANTE EL PRESENTE SUBPROYECTO EN TRES AREAS:_x000D_ (I) LA EXPLOTACION DE LA AMPLIA BASE DE DATOS ESPECTROSCOPICOS MULTIEPOCA Y MULTILONGITUD DE ONDA DE ALTA CALIDAD CONSTRUIDA DURANTE NUESTRO PROYECTO AYA PREVIO, LA BASE DE DATOS IAC DE ESTRELLAS OB, IACOB. ESTA BASE DE DATOS PERMITIRA DISCERNIR EL PAPEL DE LOS DIFERENTES PROCESOS FISICOS QUE DETERMINAN LA EVOLUCION Y EL DESTINO DE LAS ESTRELLAS MASIVAS, POR MEDIO DEL ANALISIS DE GRAN NUMERO DE ESPECTROS USANDO NUESTRAS HERRAMIENTAS DE ANALISIS AUTOMATICO, CUYA FIABILIDAD YA HEMOS COMPROBADO. PROCESOS QUE REQUIEREN ATENCION EN LA ACTUALIDAD SON EL TRANSPORTE Y PERDIDA DE MOMENTO ANGULAR, LA MULTIPLICIDAD, LAS PULSACIONES, LOS VIENTOS ESTELARES Y LOS CAMPOS MAGNETICOS. PARA OPTIMIZAR NUESTROS RESULTADOS EXTENDEREMOS NUESTRA BASE DE DATOS Y LA COMBINAREMOS CON LAS DE NUESTROS COLABORADORES (OWN, CAFE-BEANS, GOSSS), PARTICIPAREMOS EN ESFUERZOS INTERNACIONALES (VFTS, BOB, WEAVE, GES, GAIA) Y COMPARAREMOS CON MODELOS DE EVOLUCION ESTELAR CALCULADOS POR EXPERTOS INTERNACIONALES QUE COLABORAN EN NUESTRO PROYECTO. PARA ALCANZAR NUESTRO OBJETIVO UTILIZAREMOS TELESCOPIOS DE TODOS LOS TAMAÑOS, DESDE EL MERCATOR DE 1.2M AL GTC DE 10.4M, Y LA HERRAMIENTA DE CALCULO DISTRIBUIDO CONDOR._x000D_ (II) EL USO DE GALAXIAS CERCANAS COMO LABORATORIOS ESTELARES PARA EXPLORAR LA DEPENDENCIA DE LA FISICA DE LAS ESTRELLAS MASIVAS CON LA METALICIDAD Y EL ENTORNO, OBSERVANDOLAS ESPECTROSCOPICAMENTE A DISTANCIAS D<10 MPC. LOS RESULTADOS DE LOS ANALISIS SE INCORPORARAN A MODELOS DE SINTESIS DE POBLACIONES. ESTO NOS PERMITIRA EVALUAR LA FIABILIDAD DE SU EXTRAPOLACION AL UNIVERSO PRIMITIVO. EL USO DE GRANDES TELESCOPIOS Y SU INSTRUMENTACION MULTIOBJETO SERA AQUI DE IMPORTANCIA FUNDAMENTAL, PARTICULARMENTE OSIRIS Y MEGARA EN EL GTC, COMBINADOS CON NUESTRA PARTICIPACION EN CARTOGRAFIADOS INTERNACIONALES COMO LOS ARRIBA INDICADOS Y LEGUS (CON EL HST, A PARTIR DEL CUAL CONSTRUIREMOS CATALOGOS DE CANDIDATOS A ESTRELLAS MASIVAS). EN UNA ESCALA TEMPORAL MAYOR, HARMONI EN EL VLT SERA EL INSTRUMENTO REQUERIDO PARA CONTINUAR ESTA LINEA DE INVESTIGACION._x000D_ (III) LA IDENTIFICACION DE LA POBLACION DE CUMULOS ESTELARES MASIVOS EN LA VIA LACTEA, EXPLOTANDO NUESTRAS HERRAMIENTAS OPTIMIZADAS DE BUSQUEDA Y NUESTROS MODELOS ESTELARES MEJORADOS EN EL INFRARROJO CERCANO (NIR). USAREMOS LOS ESPECTROS EN EL NIR PARA REVELAR DETALLES DE LA ESTRUCTURA ESTELAR NO ACCESIBLES CON LOS ESPECTROS OPTICOS (PARTICULARMENTE, LAS INHOMOGENEIDADES EN EL VIENTO CERCA DE LA FOTOSFERA). AL MISMO TIEMPO, EVALUAREMOS LA CAPACIDAD DEL NIR PARA OBTENER PARAMETROS ESTELARES FIABLES A PARTIR TAN SOLO DE ESTE RANGO DE LONGITUD DE ONDA. LA CLAVE AQUI SERA EL USO DE ESPECTROGRAFOS MULTIOBJETO EN EL NIR, ESPECIALMENTE EMIR EN EL GTC Y KMOS EN EL VLT. (Spanish)
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MASSIVE STARS ARE KEY AGENTS IN THE CHEMICAL AND DYNAMIC EVOLUTION OF THE UNIVERSE. NOT ONLY DO THEY CONTINUOUSLY RELEASE RADIATIVE AND MECHANICAL ENERGY OVER MILLIONS OF YEARS TO THE SURROUNDING ENVIRONMENT ALONG WITH NEWLY FORMED ELEMENTS. THEY ALSO EXPLOIT AS SUPERNOVAE OF DIFFERENT TYPES WHEN THEY REACH THEIR FINAL MOMENT, INJECTING IN A FEW SECONDS COMPARABLE AMOUNTS OF ENERGY AND CONTAMINATING THE MEDIUM WITH HEAVY ELEMENTS. ITS IMPACT IS ENORMOUS DESPITE ITS SMALL NUMBER. _x000D_ our INVESTIGATION IN MASIVE STREACHS Will be focused during the present sub-project on three AREAS:_x000D_ (I) THE EXPLOTACTION OF MULTIEPOCAL Spectroscopic DATA BASE AND Multi-Length OF HIGH QUALITY CONSTRUTED DURING OUR PROJECT PREVIOUS WHY, THE BASE OF IAC DATA OF OB STRELLAS, IACOB. THIS DATABASE WILL ALLOW US TO DISCERN THE ROLE OF THE DIFFERENT PHYSICAL PROCESSES THAT DETERMINE THE EVOLUTION AND FATE OF MASSIVE STARS, THROUGH THE ANALYSIS OF A LARGE NUMBER OF SPECTRA USING OUR AUTOMATIC ANALYSIS TOOLS, THE RELIABILITY OF WHICH WE HAVE ALREADY VERIFIED. PROCESSES THAT REQUIRE ATTENTION TODAY ARE THE TRANSPORT AND LOSS OF ANGULAR MOMENTUM, MULTIPLICITY, PULSATIONS, STELLAR WINDS AND MAGNETIC FIELDS. TO OPTIMISE OUR RESULTS WE WILL EXPAND OUR DATABASE AND COMBINE IT WITH THOSE OF OUR COLLABORATORS (OWN, CAFE-BEANS, GOSSS), PARTICIPATE IN INTERNATIONAL EFFORTS (VFTS, BOB, WEAVE, GES, GAIA) AND COMPARE WITH STELLAR EVOLUTION MODELS CALCULATED BY INTERNATIONAL EXPERTS WHO COLLABORATE ON OUR PROJECT. In order to reach our OBJECTIVE, we will use telescopes of all the sizes, from the 1.2M market to the 10.4 m GTC, and the disTRIBED QALK TOOL TOOL._x000D_ (II) The use of GALAXIAS CERENCE AS THE STELLAR LABORATORIES TO EXPLORE THE DEPENDENCE OF THE FISIC OF THE MASIVE STRELLAS with metallicity and environment, noting them SPECTROSCOPICLY TO DISTANCES D<10 MPC. THE RESULTS OF THE ANALYSES WILL BE INCORPORATED INTO POPULATION SYNTHESIS MODELS. THIS WILL ALLOW US TO EVALUATE THE RELIABILITY OF ITS EXTRAPOLATION TO THE PRIMITIVE UNIVERSE. THE USE OF LARGE TELESCOPES AND THEIR MULTI-OBJECT INSTRUMENTATION WILL BE OF FUNDAMENTAL IMPORTANCE HERE, PARTICULARLY OSIRIS AND MEGARA IN THE GTC, COMBINED WITH OUR PARTICIPATION IN INTERNATIONAL MAPS SUCH AS THOSE INDICATED ABOVE AND LEGUS (WITH THE HST, FROM WHICH WE WILL BUILD CATALOGUES OF CANDIDATES FOR MASSIVE STARS). In a MAY TEMPORAL ESCAL, HARMONI IN THE VLT will be the required institution to continuate this research line._x000D_ (III) IDENTIFICATION OF THE PUBLICATION OF THE MASIVAL STELLULES IN THE LACTEA VIA, exploiting OUR OPTIMITED SEARCH TOOLS AND OUR MODELS are improved in the CERCANO INFRARROW (NIR). WE WILL USE THE SPECTRA IN THE NIR TO REVEAL DETAILS OF THE STELLAR STRUCTURE NOT ACCESSIBLE WITH THE OPTIC SPECTRA (PARTICULARLY THE INHOMOGENEITIES IN THE WIND NEAR THE PHOTOOSPHERE). AT THE SAME TIME, WE WILL EVALUATE THE ABILITY OF THE NIR TO OBTAIN RELIABLE STELLAR PARAMETERS FROM JUST THIS WAVELENGTH RANGE. THE KEY HERE WILL BE THE USE OF MULTI-OBJECT SPECTROGRAPHES IN THE NIR, ESPECIALLY EMIR IN THE GTC AND KMOS IN THE VLT. (English)
12 October 2021
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San Cristóbal de La Laguna
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Identifiers
AYA2015-68012-C2-1-P
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