Upload resources

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

 

Show simple item record

dc.date.accessioned 2020-06-02T17:54:38Z
dc.date.available 2020-06-02T17:54:38Z
dc.date.issued 2018-07
dc.identifier.uri http://sedici.unlp.edu.ar/handle/10915/97308
dc.description.abstract Context. Runaway stars produce bowshocks that are usually observed at infrared (IR) wavelengths. Non-thermal radio emission has been detected so far only from the bowshock of BD+43°3654, whereas the detection of non-thermal radiation from these bowshocks at high energies remains elusive. Aims. We aim at characterising in detail the radio, X-ray, and γ-ray emission from stellar bowshocks accounting for the structure of the region of interaction between the stellar wind and its environment. Methods. We develop a broadband-radiative, multi-zone model for stellar bowshocks that takes into account the spatial structure of the emitting region and the observational constraints. The model predicts the evolution and the emission of the relativistic particles accelerated and streaming together with the shocked flow. Results. We present broadband non-thermal spectral energy distributions for different scenarios, synthetic radio-cm synchrotron maps that reproduce the morphology of BD+43°3654, and updated predictions in X-ray and γ-ray energy ranges. We also compare the results of the multi-zone model applied in this work with those of a refined one-zone model. Conclusions. A multi-zone model provides better constraints than a one-zone model on the relevant parameters, namely the magnetic field intensity and the amount of energy deposited in non-thermal particles. However, one-zone models can be improved by carefully characterising the intensity of the IR dust photon field and the escape rate of the plasma from the shocked region. Finally, comparing observed radio maps with those obtained from a multi-zone model enables constraints to be obtained on the direction of stellar motion with respect to the observer. en
dc.format.extent 1-12 es
dc.language en es
dc.subject Acceleration of particles es
dc.subject Radiation mechanisms: non-thermal es
dc.subject Stars: massive es
dc.subject Stars: winds, outflows es
dc.title Multi-zone non-thermal radiative model for stellar bowshocks en
dc.type Articulo es
sedici.identifier.uri https://ri.conicet.gov.ar/11336/82398 es
sedici.identifier.uri https://www.aanda.org/articles/aa/abs/2018/09/aa33321-18/aa33321-18.html es
sedici.identifier.other http://dx.doi.org/10.1051/0004-6361/201833321 es
sedici.identifier.other hdl:11336/82398 es
sedici.identifier.issn 0004-6361 es
sedici.creator.person Palacio, Santiago del es
sedici.creator.person Bosch Ramon, Valentí es
sedici.creator.person Müller, Ana Laura es
sedici.creator.person Romero, Gustavo Esteban es
sedici.subject.materias Astronomía es
sedici.subject.materias Física es
sedici.subject.materias Ciencias Exactas es
sedici.description.fulltext true es
mods.originInfo.place Instituto Argentino de Radioastronomía es
mods.originInfo.place Facultad de Ciencias Astronómicas y Geofísicas es
sedici.subtype Preprint es
sedici.rights.license Creative Commons Attribution-NonCommercial-ShareAlike 2.5 Argentina (CC BY-NC-SA 2.5)
sedici.rights.uri http://creativecommons.org/licenses/by-nc-sa/2.5/ar/
sedici.description.peerReview peer-review es
sedici.relation.journalTitle Astronomy and Astrophysics es
sedici.relation.journalVolumeAndIssue vol. 617 es


Download Files

This item appears in the following Collection(s)

Creative Commons Attribution-NonCommercial-ShareAlike 2.5 Argentina (CC BY-NC-SA 2.5) Except where otherwise noted, this item's license is described as Creative Commons Attribution-NonCommercial-ShareAlike 2.5 Argentina (CC BY-NC-SA 2.5)