Geometry of the non-thermal emission in SN 1006: Azlmuthal variations of cosmic-ray acceleration

SN 1006 is the prototype of shell supernova remnants, in which non-thermal synchrotron emission dominates the X-ray spectrum. The non-thermal emission is due to the cosmic-ray electrons accelerated behind the blast wave. The X-ray synchrotron emission is due to the highest energy electrons, and is t...

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Autores principales:	Rothenflug, R., Ballet, J., Dubner, G., Giacani, E., Decourchelle, A., Ferrando, P.
Formato:	JOUR
Materias:	Acceleration of particles ISM: cosmic rays ISM: supernova remnants Magnetic fields X-rays: individuals: SN 1006 Data reduction Fourier transforms Galaxies Interferometers Magnetic field effects Mathematical models Polynomials Synchrotrons X rays ISM:cosmic rays ISM:supernova remnants X-rays:individuals:SN 1006 Cosmic rays
Acceso en línea:	http://hdl.handle.net/20.500.12110/paper_00046361_v425_n1_p121_Rothenflug
Aporte de:	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires

id	todo:paper_00046361_v425_n1_p121_Rothenflug
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spelling	todo:paper_00046361_v425_n1_p121_Rothenflug2023-10-03T14:00:08Z Geometry of the non-thermal emission in SN 1006: Azlmuthal variations of cosmic-ray acceleration Rothenflug, R. Ballet, J. Dubner, G. Giacani, E. Decourchelle, A. Ferrando, P. Acceleration of particles ISM: cosmic rays ISM: supernova remnants Magnetic fields X-rays: individuals: SN 1006 Data reduction Fourier transforms Galaxies Interferometers Magnetic field effects Mathematical models Polynomials Synchrotrons X rays Acceleration of particles ISM:cosmic rays ISM:supernova remnants X-rays:individuals:SN 1006 Cosmic rays SN 1006 is the prototype of shell supernova remnants, in which non-thermal synchrotron emission dominates the X-ray spectrum. The non-thermal emission is due to the cosmic-ray electrons accelerated behind the blast wave. The X-ray synchrotron emission is due to the highest energy electrons, and is thus a tracer of the maximum energy electrons may reach behind a shock. We have put together all XMM-Newton observations to build a full map of SN 1006. The very low brightness above 2 keV in the interior indicates that the bright non-thermal limbs are polar caps rather than an equator. This implies that the ambient magnetic field runs southwest to northeast, along the Galactic plane. We used a combined VLA/Parkes radio map to anchor the spectrum at low energy, and model the spectra with synchrotron emission from a cut-off power-law electron distribution, plus a thermal component. We present radial and azimuthal profiles of the cut-off frequency. The cut-off frequency decreases steeply with radius towards the center and with position angle away from the maximum emission. The maximum energy reached by accelerated particles, as well as their number, must be higher at the bright limbs than elsewhere. This implies interesting constraints for acceleration at perpendicular shocks. Overall the XMM-Newton data is consistent with the model in which the magnetic field is amplified where acceleration is efficient. JOUR info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_00046361_v425_n1_p121_Rothenflug
institution	Universidad de Buenos Aires
institution_str	I-28
repository_str	R-134
collection	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic	Acceleration of particles ISM: cosmic rays ISM: supernova remnants Magnetic fields X-rays: individuals: SN 1006 Data reduction Fourier transforms Galaxies Interferometers Magnetic field effects Mathematical models Polynomials Synchrotrons X rays Acceleration of particles ISM:cosmic rays ISM:supernova remnants X-rays:individuals:SN 1006 Cosmic rays
spellingShingle	Acceleration of particles ISM: cosmic rays ISM: supernova remnants Magnetic fields X-rays: individuals: SN 1006 Data reduction Fourier transforms Galaxies Interferometers Magnetic field effects Mathematical models Polynomials Synchrotrons X rays Acceleration of particles ISM:cosmic rays ISM:supernova remnants X-rays:individuals:SN 1006 Cosmic rays Rothenflug, R. Ballet, J. Dubner, G. Giacani, E. Decourchelle, A. Ferrando, P. Geometry of the non-thermal emission in SN 1006: Azlmuthal variations of cosmic-ray acceleration
topic_facet	Acceleration of particles ISM: cosmic rays ISM: supernova remnants Magnetic fields X-rays: individuals: SN 1006 Data reduction Fourier transforms Galaxies Interferometers Magnetic field effects Mathematical models Polynomials Synchrotrons X rays Acceleration of particles ISM:cosmic rays ISM:supernova remnants X-rays:individuals:SN 1006 Cosmic rays
description	SN 1006 is the prototype of shell supernova remnants, in which non-thermal synchrotron emission dominates the X-ray spectrum. The non-thermal emission is due to the cosmic-ray electrons accelerated behind the blast wave. The X-ray synchrotron emission is due to the highest energy electrons, and is thus a tracer of the maximum energy electrons may reach behind a shock. We have put together all XMM-Newton observations to build a full map of SN 1006. The very low brightness above 2 keV in the interior indicates that the bright non-thermal limbs are polar caps rather than an equator. This implies that the ambient magnetic field runs southwest to northeast, along the Galactic plane. We used a combined VLA/Parkes radio map to anchor the spectrum at low energy, and model the spectra with synchrotron emission from a cut-off power-law electron distribution, plus a thermal component. We present radial and azimuthal profiles of the cut-off frequency. The cut-off frequency decreases steeply with radius towards the center and with position angle away from the maximum emission. The maximum energy reached by accelerated particles, as well as their number, must be higher at the bright limbs than elsewhere. This implies interesting constraints for acceleration at perpendicular shocks. Overall the XMM-Newton data is consistent with the model in which the magnetic field is amplified where acceleration is efficient.
format	JOUR
author	Rothenflug, R. Ballet, J. Dubner, G. Giacani, E. Decourchelle, A. Ferrando, P.
author_facet	Rothenflug, R. Ballet, J. Dubner, G. Giacani, E. Decourchelle, A. Ferrando, P.
author_sort	Rothenflug, R.
title	Geometry of the non-thermal emission in SN 1006: Azlmuthal variations of cosmic-ray acceleration
title_short	Geometry of the non-thermal emission in SN 1006: Azlmuthal variations of cosmic-ray acceleration
title_full	Geometry of the non-thermal emission in SN 1006: Azlmuthal variations of cosmic-ray acceleration
title_fullStr	Geometry of the non-thermal emission in SN 1006: Azlmuthal variations of cosmic-ray acceleration
title_full_unstemmed	Geometry of the non-thermal emission in SN 1006: Azlmuthal variations of cosmic-ray acceleration
title_sort	geometry of the non-thermal emission in sn 1006: azlmuthal variations of cosmic-ray acceleration
url	http://hdl.handle.net/20.500.12110/paper_00046361_v425_n1_p121_Rothenflug
work_keys_str_mv	AT rothenflugr geometryofthenonthermalemissioninsn1006azlmuthalvariationsofcosmicrayacceleration AT balletj geometryofthenonthermalemissioninsn1006azlmuthalvariationsofcosmicrayacceleration AT dubnerg geometryofthenonthermalemissioninsn1006azlmuthalvariationsofcosmicrayacceleration AT giacanie geometryofthenonthermalemissioninsn1006azlmuthalvariationsofcosmicrayacceleration AT decourchellea geometryofthenonthermalemissioninsn1006azlmuthalvariationsofcosmicrayacceleration AT ferrandop geometryofthenonthermalemissioninsn1006azlmuthalvariationsofcosmicrayacceleration
_version_	1807317040943333376

Geometry of the non-thermal emission in SN 1006: Azlmuthal variations of cosmic-ray acceleration

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