The Radial Velocity Profiles of some Proplyds in the Orion Nebula
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| Format: | Artículo científico |
| Language: | en |
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Universidad Nacional Autónoma de México
2003
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| _version_ | 1876453819653554176 |
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| author | P. Ambrocio Cruz |
| author_facet | P. Ambrocio Cruz |
| contents | The Radial Velocity Profiles of some Proplyds in the Orion Nebula P. Ambrocio Cruz E. de la Fuente L. Arias Margarita Rosado Física, Astronomía y Matemáticas HII REGIONS STARS: FORMATION CIRCUMSTELLAR MATTER ISM: KINEMATICS AND DYNAMICS ISM: INDIVIDUAL (ORION NEBULA) We use H scanning Fabry-Perot interferometric data on the Orion Nebulain order to study the proplyds of the central region. We find that Fabry-Perotinterferometry constitutes an effective technique for the detection and identificationof proplyds. Some of the proplyds and proplyd candidates become noticeable onlyafter data processing of the Fabry-Perot velocity cubes. In addition, we present theH II region subtracted radial velocity profiles of most of the identified proplyds (13)and proplyd candidates (3). We estimate from these profiles their main kinematicproperties. We find that all of them have velocities redshifted relative to the Orionnebular emission. The studied proplyds show typical values of mass loss and disklifetimes and we discuss the implications of these values, taking into account the factthat this study is done over a large quantity of proplyds. Finally, we find that ourvelocity profiles suggest that a large fraction of proplyds have monopolar microjets. 2003 artículo científico 0185-1101 https://www.redalyc.org/articulo.oa?id=57139112 en http://www.redalyc.org/revista.oa?id=571 Revista Mexicana de Astronomía y Astrofísica application/pdf Universidad Nacional Autónoma de México Revista Mexicana de Astronomía y Astrofísica (México) Num.1 Vol.39 |
| format | Artículo científico |
| id | redalyc_57139112 |
| institution | Redalyc |
| language | en |
| publishDate | 2003 |
| publisher | Universidad Nacional Autónoma de México |
| spellingShingle | The Radial Velocity Profiles of some Proplyds in the Orion Nebula P. Ambrocio Cruz Física, Astronomía y Matemáticas HII REGIONS STARS: FORMATION CIRCUMSTELLAR MATTER ISM: KINEMATICS AND DYNAMICS ISM: INDIVIDUAL (ORION NEBULA) The Radial Velocity Profiles of some Proplyds in the Orion Nebula P. Ambrocio Cruz E. de la Fuente L. Arias Margarita Rosado Física, Astronomía y Matemáticas HII REGIONS STARS: FORMATION CIRCUMSTELLAR MATTER ISM: KINEMATICS AND DYNAMICS ISM: INDIVIDUAL (ORION NEBULA) We use H scanning Fabry-Perot interferometric data on the Orion Nebulain order to study the proplyds of the central region. We find that Fabry-Perotinterferometry constitutes an effective technique for the detection and identificationof proplyds. Some of the proplyds and proplyd candidates become noticeable onlyafter data processing of the Fabry-Perot velocity cubes. In addition, we present theH II region subtracted radial velocity profiles of most of the identified proplyds (13)and proplyd candidates (3). We estimate from these profiles their main kinematicproperties. We find that all of them have velocities redshifted relative to the Orionnebular emission. The studied proplyds show typical values of mass loss and disklifetimes and we discuss the implications of these values, taking into account the factthat this study is done over a large quantity of proplyds. Finally, we find that ourvelocity profiles suggest that a large fraction of proplyds have monopolar microjets. 2003 artículo científico 0185-1101 https://www.redalyc.org/articulo.oa?id=57139112 en http://www.redalyc.org/revista.oa?id=571 Revista Mexicana de Astronomía y Astrofísica application/pdf Universidad Nacional Autónoma de México Revista Mexicana de Astronomía y Astrofísica (México) Num.1 Vol.39 |
| title | The Radial Velocity Profiles of some Proplyds in the Orion Nebula |
| topic | Física, Astronomía y Matemáticas HII REGIONS STARS: FORMATION CIRCUMSTELLAR MATTER ISM: KINEMATICS AND DYNAMICS ISM: INDIVIDUAL (ORION NEBULA) |
| url | https://www.redalyc.org/articulo.oa?id=57139112 |