Collisionless shock heating of heavy ions in SN 1987A

Fabio Reale, Marco Miceli, Giovanni Peres, Costanza Argiroffi, Oleh Petruk, David N. Burrows, Kari A. Frank, Fabrizio Bocchino, Costanza Argiroffi, Fabio Reale, Salvatore Orlando, Giovanni Peres, Marco Miceli

Risultato della ricerca: Article

2 Citazioni (Scopus)

Abstract

Astrophysical shocks at all scales, from those in the helio- sphere up to cosmological shock waves, are typically ‘colli- sionless’, because the thickness of their jump region is much shorter than the collisional mean free path. Across these jumps, electrons, protons and ions are expected to be heated at different temperatures. Supernova remnants (SNRs) are ideal targets to study collisionless processes because of their bright post-shock emission and fast shocks, but the actual dependence of the post-shock temperature on the particle mass is still widely debated1. We tackle this longstanding issue through the analysis of deep multi-epoch and high-resolution observations, made with the Chandra X-ray telescope, of the youngest nearby supernova remnant, SN 1987A. We intro- duce a data analysis method by studying the observed spectra in close comparison with a dedicated full three-dimensional hydrodynamic simulation that self-consistently reproduces the broadening of the spectral lines of many ions together. We measure the post-shock temperature of protons and ions through comparison of the model with observations. Our results show that the ratio of ion temperature to proton tem- perature is always significantly higher than one and increases linearly with the ion mass for a wide range of masses and shock parameters.
Lingua originaleEnglish
pagine (da-a)236-241
Numero di pagine6
RivistaNature Astronomy
Volume3
Stato di pubblicazionePublished - 2019

Fingerprint

shock heating
heavy ions
shock
supernova remnants
protons
ions
temperature
particle mass
ion temperature
mean free path
line spectra
shock waves
astrophysics
hydrodynamics
time measurement
telescopes
high resolution

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics

Cita questo

Collisionless shock heating of heavy ions in SN 1987A. / Reale, Fabio; Miceli, Marco; Peres, Giovanni; Argiroffi, Costanza; Petruk, Oleh; Burrows, David N.; Frank, Kari A.; Bocchino, Fabrizio; Argiroffi, Costanza; Reale, Fabio; Orlando, Salvatore; Peres, Giovanni; Miceli, Marco.

In: Nature Astronomy, Vol. 3, 2019, pag. 236-241.

Risultato della ricerca: Article

Reale, F, Miceli, M, Peres, G, Argiroffi, C, Petruk, O, Burrows, DN, Frank, KA, Bocchino, F, Argiroffi, C, Reale, F, Orlando, S, Peres, G & Miceli, M 2019, 'Collisionless shock heating of heavy ions in SN 1987A', Nature Astronomy, vol. 3, pagg. 236-241.
Reale, Fabio ; Miceli, Marco ; Peres, Giovanni ; Argiroffi, Costanza ; Petruk, Oleh ; Burrows, David N. ; Frank, Kari A. ; Bocchino, Fabrizio ; Argiroffi, Costanza ; Reale, Fabio ; Orlando, Salvatore ; Peres, Giovanni ; Miceli, Marco. / Collisionless shock heating of heavy ions in SN 1987A. In: Nature Astronomy. 2019 ; Vol. 3. pagg. 236-241.
@article{5d01de3fac10498792b74fe76ba1b76a,
title = "Collisionless shock heating of heavy ions in SN 1987A",
abstract = "Astrophysical shocks at all scales, from those in the helio- sphere up to cosmological shock waves, are typically ‘colli- sionless’, because the thickness of their jump region is much shorter than the collisional mean free path. Across these jumps, electrons, protons and ions are expected to be heated at different temperatures. Supernova remnants (SNRs) are ideal targets to study collisionless processes because of their bright post-shock emission and fast shocks, but the actual dependence of the post-shock temperature on the particle mass is still widely debated1. We tackle this longstanding issue through the analysis of deep multi-epoch and high-resolution observations, made with the Chandra X-ray telescope, of the youngest nearby supernova remnant, SN 1987A. We intro- duce a data analysis method by studying the observed spectra in close comparison with a dedicated full three-dimensional hydrodynamic simulation that self-consistently reproduces the broadening of the spectral lines of many ions together. We measure the post-shock temperature of protons and ions through comparison of the model with observations. Our results show that the ratio of ion temperature to proton tem- perature is always significantly higher than one and increases linearly with the ion mass for a wide range of masses and shock parameters.",
keywords = "Astronomy and Astrophysics",
author = "Fabio Reale and Marco Miceli and Giovanni Peres and Costanza Argiroffi and Oleh Petruk and Burrows, {David N.} and Frank, {Kari A.} and Fabrizio Bocchino and Costanza Argiroffi and Fabio Reale and Salvatore Orlando and Giovanni Peres and Marco Miceli",
year = "2019",
language = "English",
volume = "3",
pages = "236--241",
journal = "Nature Astronomy",
issn = "2397-3366",
publisher = "Nature Publishing Group",

}

TY - JOUR

T1 - Collisionless shock heating of heavy ions in SN 1987A

AU - Reale, Fabio

AU - Miceli, Marco

AU - Peres, Giovanni

AU - Argiroffi, Costanza

AU - Petruk, Oleh

AU - Burrows, David N.

AU - Frank, Kari A.

AU - Bocchino, Fabrizio

AU - Argiroffi, Costanza

AU - Reale, Fabio

AU - Orlando, Salvatore

AU - Peres, Giovanni

AU - Miceli, Marco

PY - 2019

Y1 - 2019

N2 - Astrophysical shocks at all scales, from those in the helio- sphere up to cosmological shock waves, are typically ‘colli- sionless’, because the thickness of their jump region is much shorter than the collisional mean free path. Across these jumps, electrons, protons and ions are expected to be heated at different temperatures. Supernova remnants (SNRs) are ideal targets to study collisionless processes because of their bright post-shock emission and fast shocks, but the actual dependence of the post-shock temperature on the particle mass is still widely debated1. We tackle this longstanding issue through the analysis of deep multi-epoch and high-resolution observations, made with the Chandra X-ray telescope, of the youngest nearby supernova remnant, SN 1987A. We intro- duce a data analysis method by studying the observed spectra in close comparison with a dedicated full three-dimensional hydrodynamic simulation that self-consistently reproduces the broadening of the spectral lines of many ions together. We measure the post-shock temperature of protons and ions through comparison of the model with observations. Our results show that the ratio of ion temperature to proton tem- perature is always significantly higher than one and increases linearly with the ion mass for a wide range of masses and shock parameters.

AB - Astrophysical shocks at all scales, from those in the helio- sphere up to cosmological shock waves, are typically ‘colli- sionless’, because the thickness of their jump region is much shorter than the collisional mean free path. Across these jumps, electrons, protons and ions are expected to be heated at different temperatures. Supernova remnants (SNRs) are ideal targets to study collisionless processes because of their bright post-shock emission and fast shocks, but the actual dependence of the post-shock temperature on the particle mass is still widely debated1. We tackle this longstanding issue through the analysis of deep multi-epoch and high-resolution observations, made with the Chandra X-ray telescope, of the youngest nearby supernova remnant, SN 1987A. We intro- duce a data analysis method by studying the observed spectra in close comparison with a dedicated full three-dimensional hydrodynamic simulation that self-consistently reproduces the broadening of the spectral lines of many ions together. We measure the post-shock temperature of protons and ions through comparison of the model with observations. Our results show that the ratio of ion temperature to proton tem- perature is always significantly higher than one and increases linearly with the ion mass for a wide range of masses and shock parameters.

KW - Astronomy and Astrophysics

UR - http://hdl.handle.net/10447/339488

UR - https://www.nature.com/natastron/

M3 - Article

VL - 3

SP - 236

EP - 241

JO - Nature Astronomy

JF - Nature Astronomy

SN - 2397-3366

ER -