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-R120-10915-2085</identifier><datestamp>2021-04-24T04:05:06Z</datestamp>
<dc:identifier>http://sedici.unlp.edu.ar/handle/10915/2085</dc:identifier>
<dc:identifier>http://articles.adsabs.harvard.edu//full/2001ASPC..248..415C/0000415.000.html</dc:identifier>
<dc:title>Influence of magnetic in Be-stars disk formation due to rotation in line driven in stellar winds</dc:title>
<dc:creator>Curé, Michel</dc:creator>
<dc:creator>Cidale, Lydia Sonia</dc:creator>
<dc:date>2001</dc:date>
<dc:date>2010-09-27T03:00:00Z</dc:date>
<dc:language>en</dc:language>
<dc:subject>Ciencias Astronómicas</dc:subject>
<dc:subject>Geofísica, astronomía y astrofísica</dc:subject>
<dc:description>Line driven wind theory has been improved including non-spherical expansion in order to study its influence upon disk formation in early-type stars. Assuming that magnetic field controls the flow geometry, the plasma must flow downstream through open magnetic field lines. It is found that in the polar direction rapid flow tube divergence almost does not modify the location of the critical (singular) point and the calculated terminal velocity is incremented about 400 km/sec. On the other band in the equatorial direction, for a fast rotation case, the location of the critical point is unchanged and the terminal velocity shows slightly variations of about 50 km/sec. This conclusion is the polar direction is contrary to previous results, where the finite disk correction has not been taken into account. These results suggest, that open magnetic field lines do not influence disk formation in Be-stars.</dc:description>
<dc:description>Facultad de Ciencias Astronómicas y Geofísicas</dc:description>
<dc:type>Articulo</dc:type>
<dc:type>Articulo</dc:type>
<dc:rights>http://creativecommons.org/licenses/by-nc-nd/4.0/</dc:rights>
<dc:rights>Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International (CC BY-NC-ND 4.0)</dc:rights>
<dc:format>application/pdf</dc:format>
<dc:format>415-418</dc:format>
</oai_dc:dc>

Datos convertidos

{
    "id": "I19-R120-10915-2085",
    "record_format": "dspace",
    "spelling": [
        "I19-R120-10915-20852021-04-24T04:05:06Z http:\/\/sedici.unlp.edu.ar\/handle\/10915\/2085 http:\/\/articles.adsabs.harvard.edu\/\/full\/2001ASPC..248..415C\/0000415.000.html Influence of magnetic in Be-stars disk formation due to rotation in line driven in stellar winds Cur\u00e9, Michel Cidale, Lydia Sonia 2001 2010-09-27T03:00:00Z en Ciencias Astron\u00f3micas Geof\u00edsica, astronom\u00eda y astrof\u00edsica Line driven wind theory has been improved including non-spherical expansion in order to study its influence upon disk formation in early-type stars. Assuming that magnetic field controls the flow geometry, the plasma must flow downstream through open magnetic field lines. It is found that in the polar direction rapid flow tube divergence almost does not modify the location of the critical (singular) point and the calculated terminal velocity is incremented about 400 km\/sec. On the other band in the equatorial direction, for a fast rotation case, the location of the critical point is unchanged and the terminal velocity shows slightly variations of about 50 km\/sec. This conclusion is the polar direction is contrary to previous results, where the finite disk correction has not been taken into account. These results suggest, that open magnetic field lines do not influence disk formation in Be-stars. Facultad de Ciencias Astron\u00f3micas y Geof\u00edsicas Articulo Articulo http:\/\/creativecommons.org\/licenses\/by-nc-nd\/4.0\/ Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International (CC BY-NC-ND 4.0) application\/pdf 415-418"
    ],
    "institution": [
        "Universidad Nacional de La Plata"
    ],
    "institution_str": "I-19",
    "repository_str": "R-120",
    "collection": [
        "SEDICI (UNLP)"
    ],
    "language": [
        "Ingl\u00e9s"
    ],
    "topic": [
        "Ciencias Astron\u00f3micas",
        "Geof\u00edsica, astronom\u00eda y astrof\u00edsica"
    ],
    "spellingShingle": [
        "Ciencias Astron\u00f3micas",
        "Geof\u00edsica, astronom\u00eda y astrof\u00edsica",
        "Cur\u00e9, Michel",
        "Cidale, Lydia Sonia",
        "Influence of magnetic in Be-stars disk formation due to rotation in line driven in stellar winds"
    ],
    "topic_facet": [
        "Ciencias Astron\u00f3micas",
        "Geof\u00edsica, astronom\u00eda y astrof\u00edsica"
    ],
    "description": "Line driven wind theory has been improved including non-spherical expansion in order to study its influence upon disk formation in early-type stars. Assuming that magnetic field controls the flow geometry, the plasma must flow downstream through open magnetic field lines. It is found that in the polar direction rapid flow tube divergence almost does not modify the location of the critical (singular) point and the calculated terminal velocity is incremented about 400 km\/sec. On the other band in the equatorial direction, for a fast rotation case, the location of the critical point is unchanged and the terminal velocity shows slightly variations of about 50 km\/sec. This conclusion is the polar direction is contrary to previous results, where the finite disk correction has not been taken into account. These results suggest, that open magnetic field lines do not influence disk formation in Be-stars.",
    "format": [
        "Articulo",
        "Articulo"
    ],
    "author": [
        "Cur\u00e9, Michel",
        "Cidale, Lydia Sonia"
    ],
    "author_facet": [
        "Cur\u00e9, Michel",
        "Cidale, Lydia Sonia"
    ],
    "author_sort": "Cur\u00e9, Michel",
    "title": "Influence of magnetic in Be-stars disk formation due to rotation in line driven in stellar winds",
    "title_short": "Influence of magnetic in Be-stars disk formation due to rotation in line driven in stellar winds",
    "title_full": "Influence of magnetic in Be-stars disk formation due to rotation in line driven in stellar winds",
    "title_fullStr": "Influence of magnetic in Be-stars disk formation due to rotation in line driven in stellar winds",
    "title_full_unstemmed": "Influence of magnetic in Be-stars disk formation due to rotation in line driven in stellar winds",
    "title_sort": "influence of magnetic in be-stars disk formation due to rotation in line driven in stellar winds",
    "publishDate": [
        "2001"
    ],
    "url": [
        "http:\/\/sedici.unlp.edu.ar\/handle\/10915\/2085",
        "http:\/\/articles.adsabs.harvard.edu\/\/full\/2001ASPC..248..415C\/0000415.000.html"
    ],
    "work_keys_str_mv": [
        "AT curemichel influenceofmagneticinbestarsdiskformationduetorotationinlinedriveninstellarwinds",
        "AT cidalelydiasonia influenceofmagneticinbestarsdiskformationduetorotationinlinedriveninstellarwinds"
    ],
    "_version_": 1734111904929939456
}