Supernova Remnants Interacting with Molecular Clouds: X-Ray and Gamma-Ray Signatures
The giant molecular clouds (MCs) found in the Milky Way and similar galaxies play a crucial role in the evolution of these systems. The supernova explosions that mark the death of massive stars in these regions often lead to interactions between the supernova remnants (SNRs) and the clouds. These in...
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2015
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| Acceso en línea: | https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00386308_v188_n1-4_p187_Slane http://hdl.handle.net/20.500.12110/paper_00386308_v188_n1-4_p187_Slane |
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paper:paper_00386308_v188_n1-4_p187_Slane2023-06-08T15:03:05Z Supernova Remnants Interacting with Molecular Clouds: X-Ray and Gamma-Ray Signatures Gamma-rays Molecular clouds Supernova remnants X-rays Astronomy Clouds Cosmic rays Galaxies Supernovae X rays Acceleration mechanisms Diffusive shock accelerations Dynamical evolution Giant molecular clouds Molecular clouds Relativistic electron Supernova explosion Supernova remnants Gamma rays The giant molecular clouds (MCs) found in the Milky Way and similar galaxies play a crucial role in the evolution of these systems. The supernova explosions that mark the death of massive stars in these regions often lead to interactions between the supernova remnants (SNRs) and the clouds. These interactions have a profound effect on our understanding of SNRs. Shocks in SNRs should be capable of accelerating particles to cosmic ray (CR) energies with efficiencies high enough to power Galactic CRs. X-ray and γ-ray studies have established the presence of relativistic electrons and protons in some SNRs and provided strong evidence for diffusive shock acceleration as the primary acceleration mechanism, including strongly amplified magnetic fields, temperature and ionization effects on the shock-heated plasmas, and modifications to the dynamical evolution of some systems. Because protons dominate the overall energetics of the CRs, it is crucial to understand this hadronic component even though electrons are much more efficient radiators and it can be difficult to identify the hadronic component. However, near MCs the densities are sufficiently high to allow the γ-ray emission to be dominated by protons. Thus, these interaction sites provide some of our best opportunities to constrain the overall energetics of these particle accelerators. Here we summarize some key properties of interactions between SNRs and MCs, with an emphasis on recent X-ray and γ-ray studies that are providing important constraints on our understanding of cosmic rays in our Galaxy. © 2014, Springer Science+Business Media Dordrecht. 2015 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00386308_v188_n1-4_p187_Slane http://hdl.handle.net/20.500.12110/paper_00386308_v188_n1-4_p187_Slane |
| institution |
Universidad de Buenos Aires |
| institution_str |
I-28 |
| repository_str |
R-134 |
| collection |
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) |
| topic |
Gamma-rays Molecular clouds Supernova remnants X-rays Astronomy Clouds Cosmic rays Galaxies Supernovae X rays Acceleration mechanisms Diffusive shock accelerations Dynamical evolution Giant molecular clouds Molecular clouds Relativistic electron Supernova explosion Supernova remnants Gamma rays |
| spellingShingle |
Gamma-rays Molecular clouds Supernova remnants X-rays Astronomy Clouds Cosmic rays Galaxies Supernovae X rays Acceleration mechanisms Diffusive shock accelerations Dynamical evolution Giant molecular clouds Molecular clouds Relativistic electron Supernova explosion Supernova remnants Gamma rays Supernova Remnants Interacting with Molecular Clouds: X-Ray and Gamma-Ray Signatures |
| topic_facet |
Gamma-rays Molecular clouds Supernova remnants X-rays Astronomy Clouds Cosmic rays Galaxies Supernovae X rays Acceleration mechanisms Diffusive shock accelerations Dynamical evolution Giant molecular clouds Molecular clouds Relativistic electron Supernova explosion Supernova remnants Gamma rays |
| description |
The giant molecular clouds (MCs) found in the Milky Way and similar galaxies play a crucial role in the evolution of these systems. The supernova explosions that mark the death of massive stars in these regions often lead to interactions between the supernova remnants (SNRs) and the clouds. These interactions have a profound effect on our understanding of SNRs. Shocks in SNRs should be capable of accelerating particles to cosmic ray (CR) energies with efficiencies high enough to power Galactic CRs. X-ray and γ-ray studies have established the presence of relativistic electrons and protons in some SNRs and provided strong evidence for diffusive shock acceleration as the primary acceleration mechanism, including strongly amplified magnetic fields, temperature and ionization effects on the shock-heated plasmas, and modifications to the dynamical evolution of some systems. Because protons dominate the overall energetics of the CRs, it is crucial to understand this hadronic component even though electrons are much more efficient radiators and it can be difficult to identify the hadronic component. However, near MCs the densities are sufficiently high to allow the γ-ray emission to be dominated by protons. Thus, these interaction sites provide some of our best opportunities to constrain the overall energetics of these particle accelerators. Here we summarize some key properties of interactions between SNRs and MCs, with an emphasis on recent X-ray and γ-ray studies that are providing important constraints on our understanding of cosmic rays in our Galaxy. © 2014, Springer Science+Business Media Dordrecht. |
| title |
Supernova Remnants Interacting with Molecular Clouds: X-Ray and Gamma-Ray Signatures |
| title_short |
Supernova Remnants Interacting with Molecular Clouds: X-Ray and Gamma-Ray Signatures |
| title_full |
Supernova Remnants Interacting with Molecular Clouds: X-Ray and Gamma-Ray Signatures |
| title_fullStr |
Supernova Remnants Interacting with Molecular Clouds: X-Ray and Gamma-Ray Signatures |
| title_full_unstemmed |
Supernova Remnants Interacting with Molecular Clouds: X-Ray and Gamma-Ray Signatures |
| title_sort |
supernova remnants interacting with molecular clouds: x-ray and gamma-ray signatures |
| publishDate |
2015 |
| url |
https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00386308_v188_n1-4_p187_Slane http://hdl.handle.net/20.500.12110/paper_00386308_v188_n1-4_p187_Slane |
| _version_ |
1768545684155269120 |