Upload resources

Upload your works to SEDICI to increase its visibility and improve its impact

 

Show simple item record

dc.date.accessioned 2019-11-01T12:41:29Z
dc.date.available 2019-11-01T12:41:29Z
dc.date.issued 2012-10
dc.identifier.uri http://sedici.unlp.edu.ar/handle/10915/84599
dc.description.abstract Context. The origin and evolution of supernova remnants of the mixed-morphology class is not well understood. Several remnants present distorted radio or X-ray shells with jet-like structures. G290.1-0.8 (MSH 11-61A) belongs to this particular class. Aims. We aim to investigate the nature of this supernova remnant in order to unveil the origin of its particular morphology. We based our work on the study of the X-ray emitting plasma properties and the conditions imposed by the cold interstellar medium where the remnant expanded. Methods. We use archival radio, H I line data and X-ray observations from XMM-Newton and Chandra observatories, to study G290.1-0.8 and its surrounding medium in detail. Spatially resolved spectral analysis and mean photon energy maps are used to obtain physical and geometrical parameters of the source. Radio continuum and H I line maps give crucial information to understand the radio/X-ray morphology. Results. The X-ray images show that the supernova remnant presents two opposite symmetric bright spots on a symmetry axis running towards the north west-south east direction. Spectral analysis and mean photon energy maps confirm that the physical conditions of the emitting plasma are not homogeneous throughout the remnant. In fact, both bright spots have higher temperatures than the rest of the plasma and its constituents have not reached ionization equilibrium yet. H I line data reveal low density tube-like structures aligned along the same direction. This evidence supports the idea that the particular X-ray morphology observed is a direct consequence of the structure of the interstellar medium where the remnant evolved. However, the possibility that an undetected point-like object, as a neutron star, exists within the remnant and contributes to the X-ray emission cannot be discarded. Finally, we suggest that a supernova explosion due to the collapse of a high-mass star with a strong bipolar wind can explain the supernova remnant morphology. en
dc.language en es
dc.subject Rayos X es
dc.subject ISM: individual objects: G290.1 es
dc.subject ISM: supernova remnants es
dc.subject Radiation mechanisms: thermal es
dc.subject X-rays: ISM es
dc.subject G290.1–0.8 es
dc.title On the origin of the jet-like radio/X-ray morphology of G290.1-0.8 en
dc.type Articulo es
sedici.identifier.other https://doi.org/10.1051/0004-6361/201218959 es
sedici.identifier.issn 0004-6361 es
sedici.creator.person García, Federico es
sedici.creator.person Combi, Jorge Ariel es
sedici.creator.person Albacete Colombo, Juan Facundo es
sedici.creator.person Romero, Gustavo Esteban es
sedici.creator.person Bocchino, F. es
sedici.creator.person López Santiago, J. es
sedici.subject.materias Ciencias Astronómicas es
sedici.description.fulltext true es
mods.originInfo.place Facultad de Ciencias Astronómicas y Geofísicas es
sedici.subtype Articulo es
sedici.rights.license Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
sedici.rights.uri http://creativecommons.org/licenses/by-nc-sa/4.0/
sedici.description.peerReview peer-review es
sedici.relation.journalTitle Astronomy and Astrophysics es
sedici.relation.journalVolumeAndIssue vol. 546 es
sedici.rights.sherpa * Color: verde* Pre-print del autor: si* Post-print del autor: si* Versión de editor/PDF:si* Condiciones:>>En el sitio web del autor o institucional o sitios que cumplan las directrices OAI>>Algunas revistas requieren un periodo de embargo para su depósito en repositorios recomendados por los organismos financiadores (ver revista)>>La versión de editor/PDF puede utilizarse (ver revista)>>Debe ir enlazado a la versión de editor>>Deben reconocerse el copyright y la fuente editorial>>No comercial* Link a Sherpa: http://sherpa.ac.uk/romeo/issn/0004-6361/es/


Download Files

This item appears in the following Collection(s)

Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0) Except where otherwise noted, this item's license is described as Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)