Herramienta de chequeo de registro xml obtenido desde SEDICI (UNLP)

XML

<oai_dc:dc xmlns:oai_dc="http://www.openarchives.org/OAI/2.0/oai_dc/" xmlns:doc="http://www.lyncode.com/xoai" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xmlns:dc="http://purl.org/dc/elements/1.1/" xsi:schemaLocation="http://www.openarchives.org/OAI/2.0/oai_dc/ http://www.openarchives.org/OAI/2.0/oai_dc.xsd"><identifier>I19-R120-10915-84055</identifier><datestamp>2020-02-25T04:06:04Z</datestamp>
<dc:identifier>http://sedici.unlp.edu.ar/handle/10915/84055</dc:identifier>
<dc:identifier>issn:1743-9213</dc:identifier>
<dc:title>Radiation driven winds with rotation: the oblate finite disc correction factor</dc:title>
<dc:creator>Araya, Ignacio</dc:creator>
<dc:creator>Curé, Michel</dc:creator>
<dc:creator>Granada, Anahí</dc:creator>
<dc:creator>Cidale, Lydia Sonia</dc:creator>
<dc:date>2011-07-12</dc:date>
<dc:date>2019-10-25T14:05:55Z</dc:date>
<dc:language>en</dc:language>
<dc:subject>Ciencias Astronómicas</dc:subject>
<dc:subject>Ciencias Exactas</dc:subject>
<dc:subject>Be</dc:subject>
<dc:subject>Outflows</dc:subject>
<dc:subject>Stars: early-type</dc:subject>
<dc:subject>Stars: emission-line</dc:subject>
<dc:subject>Stars: rotation</dc:subject>
<dc:subject>Stars: winds</dc:subject>
<dc:description>We have incorporated the oblate distortion of the shape of the star due to the stellar rotation, which modifies the finite disk correction factor (f D) in the m-CAK hydrodynamical model. We implement a simplified version for the fD allowing us to solve numerically the non-linear m-CAK momentum equation. We solve this model for a classical Be star in the polar and equatorial directions. The star's oblateness modifies the polar wind, which is now much faster than the spherical one, mainly because the wind receives radiation from a larger (than the spherical) stellar surface. In the equatorial direction we obtain slow solutions, which are even slower and denser than the spherical ones. For the case when the stellar rotational velocity is about the critical velocity, the most remarkable result of our calculations is that the density contrast between the equatorial density and the polar one, is about 100. This result could explain a long-standing problem on Be stars.</dc:description>
<dc:description>Facultad de Ciencias Astronómicas y Geofísicas</dc:description>
<dc:type>Articulo</dc:type>
<dc:type>Preprint</dc:type>
<dc:rights>http://creativecommons.org/licenses/by-nc-sa/4.0/</dc:rights>
<dc:rights>Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)</dc:rights>
<dc:format>application/pdf</dc:format>
<dc:format>83-84</dc:format>
</oai_dc:dc>

Datos convertidos

{
    "id": "I19-R120-10915-84055",
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    "spelling": [
        "I19-R120-10915-840552020-02-25T04:06:04Z http:\/\/sedici.unlp.edu.ar\/handle\/10915\/84055 issn:1743-9213 Radiation driven winds with rotation: the oblate finite disc correction factor Araya, Ignacio Cur\u00e9, Michel Granada, Anah\u00ed Cidale, Lydia Sonia 2011-07-12 2019-10-25T14:05:55Z en Ciencias Astron\u00f3micas Ciencias Exactas Be Outflows Stars: early-type Stars: emission-line Stars: rotation Stars: winds We have incorporated the oblate distortion of the shape of the star due to the stellar rotation, which modifies the finite disk correction factor (f D) in the m-CAK hydrodynamical model. We implement a simplified version for the fD allowing us to solve numerically the non-linear m-CAK momentum equation. We solve this model for a classical Be star in the polar and equatorial directions. The star's oblateness modifies the polar wind, which is now much faster than the spherical one, mainly because the wind receives radiation from a larger (than the spherical) stellar surface. In the equatorial direction we obtain slow solutions, which are even slower and denser than the spherical ones. For the case when the stellar rotational velocity is about the critical velocity, the most remarkable result of our calculations is that the density contrast between the equatorial density and the polar one, is about 100. This result could explain a long-standing problem on Be stars. Facultad de Ciencias Astron\u00f3micas y Geof\u00edsicas Articulo Preprint http:\/\/creativecommons.org\/licenses\/by-nc-sa\/4.0\/ Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0) application\/pdf 83-84"
    ],
    "institution": [
        "Universidad Nacional de La Plata"
    ],
    "institution_str": "I-19",
    "repository_str": "R-120",
    "collection": [
        "SEDICI (UNLP)"
    ],
    "language": [
        "Ingl\u00e9s"
    ],
    "topic": [
        "Ciencias Astron\u00f3micas",
        "Ciencias Exactas",
        "Be",
        "Outflows",
        "Stars: early-type",
        "Stars: emission-line",
        "Stars: rotation",
        "Stars: winds"
    ],
    "spellingShingle": [
        "Ciencias Astron\u00f3micas",
        "Ciencias Exactas",
        "Be",
        "Outflows",
        "Stars: early-type",
        "Stars: emission-line",
        "Stars: rotation",
        "Stars: winds",
        "Araya, Ignacio",
        "Cur\u00e9, Michel",
        "Granada, Anah\u00ed",
        "Cidale, Lydia Sonia",
        "Radiation driven winds with rotation: the oblate finite disc correction factor"
    ],
    "topic_facet": [
        "Ciencias Astron\u00f3micas",
        "Ciencias Exactas",
        "Be",
        "Outflows",
        "Stars: early-type",
        "Stars: emission-line",
        "Stars: rotation",
        "Stars: winds"
    ],
    "description": "We have incorporated the oblate distortion of the shape of the star due to the stellar rotation, which modifies the finite disk correction factor (f D) in the m-CAK hydrodynamical model. We implement a simplified version for the fD allowing us to solve numerically the non-linear m-CAK momentum equation. We solve this model for a classical Be star in the polar and equatorial directions. The star's oblateness modifies the polar wind, which is now much faster than the spherical one, mainly because the wind receives radiation from a larger (than the spherical) stellar surface. In the equatorial direction we obtain slow solutions, which are even slower and denser than the spherical ones. For the case when the stellar rotational velocity is about the critical velocity, the most remarkable result of our calculations is that the density contrast between the equatorial density and the polar one, is about 100. This result could explain a long-standing problem on Be stars.",
    "format": [
        "Articulo",
        "Preprint"
    ],
    "author": [
        "Araya, Ignacio",
        "Cur\u00e9, Michel",
        "Granada, Anah\u00ed",
        "Cidale, Lydia Sonia"
    ],
    "author_facet": [
        "Araya, Ignacio",
        "Cur\u00e9, Michel",
        "Granada, Anah\u00ed",
        "Cidale, Lydia Sonia"
    ],
    "author_sort": "Araya, Ignacio",
    "title": "Radiation driven winds with rotation: the oblate finite disc correction factor",
    "title_short": "Radiation driven winds with rotation: the oblate finite disc correction factor",
    "title_full": "Radiation driven winds with rotation: the oblate finite disc correction factor",
    "title_fullStr": "Radiation driven winds with rotation: the oblate finite disc correction factor",
    "title_full_unstemmed": "Radiation driven winds with rotation: the oblate finite disc correction factor",
    "title_sort": "radiation driven winds with rotation: the oblate finite disc correction factor",
    "publishDate": [
        "2011"
    ],
    "url": [
        "http:\/\/sedici.unlp.edu.ar\/handle\/10915\/84055"
    ],
    "work_keys_str_mv": [
        "AT arayaignacio radiationdrivenwindswithrotationtheoblatefinitedisccorrectionfactor",
        "AT curemichel radiationdrivenwindswithrotationtheoblatefinitedisccorrectionfactor",
        "AT granadaanahi radiationdrivenwindswithrotationtheoblatefinitedisccorrectionfactor",
        "AT cidalelydiasonia radiationdrivenwindswithrotationtheoblatefinitedisccorrectionfactor"
    ],
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}