Non-Thermal Radio and Gamma-Ray Emissions from a Supernova Remnant by Blast Wave Breaking Out of the Circumstellar Matter
Non-Thermal Radio and Gamma-Ray Emissions from a Supernova Remnant by Blast Wave Breaking Out of the Circumstellar Matter
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超新星遗迹由星周物质爆发的爆炸波产生的非热射电和伽马射线发射
DOI：
10.1093/pasj/65.3.69
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发表时间：
2013
影响因子：
2.3
通讯作者：
K. Koyama
中科院分区：
文献类型：
--
作者：
Takafumi Shimizu;K. Masai;K. Koyama
本文计算了超新星遗迹在其前身星风形成的星周物质中爆炸产生的韧致辐射、逆康普顿散射和π ^0 $-衰变引起的同步辐射和γ射线辐射。这种情况可能是像W 49 B这样的混合形态超新星遗迹（SNRs）的起源，它们在X射线发射中表现出复合辐射光谱。我们假定在密度为0.016 cm-3的星际介质中，距离超新星0.07- 3 pc处存在着1.5 M_（odot）的CSM。当冲击波冲出CSM进入ISM时，其速度迅速增加，因此颗粒加速增强。爆发后质子的最大能量达到1300 TeV，仅为爆炸能量的0.5%。我们考虑了爆炸冲击后ISM壳体的非热辐射。在1 GHz的同步辐射通量是几十焦耳，可比观察到的混合形态信噪比。由于密度低，伽马射线的光度主要由逆康普顿散射决定，它比衰变光度高一个数量级。包括韧致辐射在内的伽马射线总光度比从混合形态信噪比观测到的典型值10 ^{35}$-10 ^{36}$erg s$^{-1}$低10 ^{33}$ erg s$^{-1}$。然而，如果，例如，10%的加速质子与密度为100 cm ^{-3}$，pi ^0 $的物质相互作用，衰变伽马射线的亮度将提高到与观测值相当。
We calculate synchrotron radio emission and gamma-ray emission due to bremsstrahlung, inverse-Compton scattering and $pi^0$-decay from the remnant of supernova which exploded in the circumstellar matter (CSM) formed by the progenitor's stellar wind. This sort of situation is a possible origin of mixed-morphology supernova remnants (SNRs) like W49B, which exhibit recombination-radiation spectra in X-ray emission. We assume that the CSM of 1.5 $M_{odot}$ exists at 0.07--3 pc away from the supernova in the interstellar medium (ISM) of density 0.016 cm$^{-3}$. When the blast wave breaks out of the CSM into the ISM, its velocity rapidly increases and hence particle acceleration is enhanced. The maximum energy of protons reaches $sim$ 1300 TeV just after the break-out with $sim$ 0.5% of the explosion energy. We consider the non-thermal emission from the blast-shocked ISM shell after the break-out. Synchrotron radio flux at 1 GHz is tens Jy, comparable to the observed from mixed-morphology SNRs. Because of low density, the gamma-ray luminosity is dominated by inverse-Compton scattering, which is higher than the $pi^0$-decay luminosity by an order of magnitude. The total gamma-ray luminosity including bremsstrahlung is of the order of $10^{33}$ erg s$^{-1}$ lower than the typical value $10^{35}$--$10^{36}$ erg s$^{-1}$ observed from mixed-morphology SNRs. However, if, e.g., $sim$10% of accelerated protons interact with some matter of density $sim$100 cm$^{-3}$, $pi^0$-decay gamma-ray luminosity would be enhanced to be comparable with the observed value.
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DOI：
10.1088/0004-637x/705/1/l6
发表时间：
2009-09
期刊：
The Astrophysical Journal
影响因子：
--
作者：
H. Yamaguchi;M. Ozawa;K. Koyama;K. Masai;J. Hiraga;M. Ozaki;D. Yonetoku
通讯作者：
H. Yamaguchi;M. Ozawa;K. Koyama;K. Masai;J. Hiraga;M. Ozaki;D. Yonetoku
DOI：
10.1086/588499
发表时间：
2008-03
期刊：
The Astrophysical Journal Letters
影响因子：
--
作者：
S. Katsuda;H. Tsunemi;K. Mori
通讯作者：
S. Katsuda;H. Tsunemi;K. Mori
DOI：
10.1088/0004-637x/706/1/l1
发表时间：
2009-10
期刊：
The Astrophysical Journal
影响因子：
--
作者：
A. Abdo;M. Ackermann;M. Ajello;L. Baldini;J. Ballet;G. Barbiellini;M. Baring;D. Bastieri;B. Baughman;K. Bechtol;R. Bellazzini;B. Berenji;R. Blandford;E. Bloom;E. Bonamente;A. Borgland;A. Bouvier;J. Bregeon;A. Brez;M. Brigida;P. Bruel;T. Burnett;S. Buson;G. Caliandro;R. Cameron;P. Caraveo;J. Casandjian;C. Cecchi;O. Celik;A. Chekhtman;C. C. Cheung-C.;J. Chiang;S. Ciprini;R. Claus;J. Cohen-Tanugi;L. Cominsky;J. Conrad;S. Cutini;C. Dermer;A. Angelis;F. Palma;S. Digel;M. Dormody;E. Silva;P. Drell;R. Dubois;D. Dumora;C. Farnier;C. Favuzzi;S. Fegan;W. Focke;P. Fortin;M. Frailis;Y. Fukazawa;S. Funk;P. Fusco;F. Gargano;D. Gasparrini;N. Gehrels;S. Germani;G. Giavitto;B. Giebels;N. Giglietto;F. Giordano;T. Glanzman;G. Godfrey;I. Grenier;M. Grondin;J. Grove;L. Guillemot;S. Guiriec;Y. Hanabata;A. Harding;M. Hayashida;E. Hays;R. Hughes;M. Jackson;G. Jóhannesson;A. Johnson;T. Johnson;W. Johnson;T. Kamae;H. Katagiri;J. Kataoka;J. Katsuta;N. Kawai;M. Kerr;J. Knödlseder;M. Kocián;M. Kuss;J. Lande;L. Latronico;M. Lemoine-Goumard;F. Longo;F. Loparco;B. Lott;M. Lovellette;P. Lubrano;A. Makeev;M. Mazziotta;J. Mcenery;C. Meurer;P. Michelson;W. Mitthumsiri;T. Mizuno;A. Moiseev;C. Monte;M. Monzani;A. Morselli;I. Moskalenko;S. Murgia;T. Nakamori;P. Nolan;J. Norris;E. Nuss;T. Ohsugi;A. Okumura;N. Omodei;E. Orlando;J. Ormes;D. Paneque;D. Parent;V. Pelassa;M. Pepe;M. Pesce-Rollins;F. Piron;T. Porter;S. Rainò;R. Rando;M. Razzano;A. Reimer;O. Reimer;T. Reposeur;S. Ritz;A. Rodríguez;R. Romani;M. Roth;F. Ryde;H. Sadrozinski;D. Sanchez;A. Sander;P. Parkinson;J. Scargle;T. Schalk;C. Sgro’;E. Siskind;D. Smith;P. Smith;G. Spandre;P. Spinelli;M. Strickman;D. Suson;H. Tajima;H. Takahashi;Tadayuki Takahashi;Takaaki Tanaka;J. Thayer;J. Thayer;D. Thompson;L. Tibaldo;O. Tibolla;D. Torres;G. Tosti;A. Tramacere;Y. Uchiyama;T. Usher;V. Vasileiou;C. Venter;N. Vilchez;V. Vitale;A. Waite;Pengfei Wang;B. Winer;K. Wood;R. Yamazaki;T. Ylinen;M. Ziegler
通讯作者：
A. Abdo;M. Ackermann;M. Ajello;L. Baldini;J. Ballet;G. Barbiellini;M. Baring;D. Bastieri;B. Baughman;K. Bechtol;R. Bellazzini;B. Berenji;R. Blandford;E. Bloom;E. Bonamente;A. Borgland;A. Bouvier;J. Bregeon;A. Brez;M. Brigida;P. Bruel;T. Burnett;S. Buson;G. Caliandro;R. Cameron;P. Caraveo;J. Casandjian;C. Cecchi;O. Celik;A. Chekhtman;C. C. Cheung-C.;J. Chiang;S. Ciprini;R. Claus;J. Cohen-Tanugi;L. Cominsky;J. Conrad;S. Cutini;C. Dermer;A. Angelis;F. Palma;S. Digel;M. Dormody;E. Silva;P. Drell;R. Dubois;D. Dumora;C. Farnier;C. Favuzzi;S. Fegan;W. Focke;P. Fortin;M. Frailis;Y. Fukazawa;S. Funk;P. Fusco;F. Gargano;D. Gasparrini;N. Gehrels;S. Germani;G. Giavitto;B. Giebels;N. Giglietto;F. Giordano;T. Glanzman;G. Godfrey;I. Grenier;M. Grondin;J. Grove;L. Guillemot;S. Guiriec;Y. Hanabata;A. Harding;M. Hayashida;E. Hays;R. Hughes;M. Jackson;G. Jóhannesson;A. Johnson;T. Johnson;W. Johnson;T. Kamae;H. Katagiri;J. Kataoka;J. Katsuta;N. Kawai;M. Kerr;J. Knödlseder;M. Kocián;M. Kuss;J. Lande;L. Latronico;M. Lemoine-Goumard;F. Longo;F. Loparco;B. Lott;M. Lovellette;P. Lubrano;A. Makeev;M. Mazziotta;J. Mcenery;C. Meurer;P. Michelson;W. Mitthumsiri;T. Mizuno;A. Moiseev;C. Monte;M. Monzani;A. Morselli;I. Moskalenko;S. Murgia;T. Nakamori;P. Nolan;J. Norris;E. Nuss;T. Ohsugi;A. Okumura;N. Omodei;E. Orlando;J. Ormes;D. Paneque;D. Parent;V. Pelassa;M. Pepe;M. Pesce-Rollins;F. Piron;T. Porter;S. Rainò;R. Rando;M. Razzano;A. Reimer;O. Reimer;T. Reposeur;S. Ritz;A. Rodríguez;R. Romani;M. Roth;F. Ryde;H. Sadrozinski;D. Sanchez;A. Sander;P. Parkinson;J. Scargle;T. Schalk;C. Sgro’;E. Siskind;D. Smith;P. Smith;G. Spandre;P. Spinelli;M. Strickman;D. Suson;H. Tajima;H. Takahashi;Tadayuki Takahashi;Takaaki Tanaka;J. Thayer;J. Thayer;D. Thompson;L. Tibaldo;O. Tibolla;D. Torres;G. Tosti;A. Tramacere;Y. Uchiyama;T. Usher;V. Vasileiou;C. Venter;N. Vilchez;V. Vitale;A. Waite;Pengfei Wang;B. Winer;K. Wood;R. Yamazaki;T. Ylinen;M. Ziegler
DOI：
10.1088/0004-637x/712/1/459
发表时间：
2010-02
期刊：
The Astrophysical Journal
影响因子：
--
作者：
A. Abdo;A. Abdo;A. Abdo;M. Ackermann;M. Ajello;L. Baldini;J. Ballet;G. Barbiellini;G. Barbiellini;D. Bastieri;D. Bastieri;B. Baughman;K. Bechtol;R. Bellazzini;B. Berenji;R. Blandford;E. Bloom;E. Bonamente;E. Bonamente;A. Borgland;J. Bregeon;A. Brez;M. Brigida;M. Brigida;P. Bruel;T. Burnett;S. Buson;G. Caliandro;G. Caliandro;R. Cameron;P. Caraveo;J. Casandjian;C. Cecchi;C. Cecchi;O. Celik;O. Celik;A. Chekhtman;A. Chekhtman;C. C. Cheung-C.;J. Chiang;A. Cillis;S. Ciprini;S. Ciprini;R. Claus;J. Cohen-Tanugi;L. Cominsky;J. Conrad;J. Conrad;S. Cutini;C. Dermer;A. Angelis;F. Palma;F. Palma;E. Silva;P. Drell;A. Drlica-Wagner;R. Dubois;D. Dumora;D. Dumora;C. Farnier;C. Favuzzi;C. Favuzzi;S. Fegan;W. Focke;P. Fortin;M. Frailis;Y. Fukazawa;S. Funk;P. Fusco;P. Fusco;F. Gargano;D. Gasparrini;N. Gehrels;N. Gehrels;S. Germani;S. Germani;G. Giavitto;B. Giebels;N. Giglietto;N. Giglietto;F. Giordano;F. Giordano;T. Glanzman;G. Godfrey;I. Grenier;M. Grondin;M. Grondin;J. Grove;L. Guillemot;L. Guillemot;S. Guiriec;Y. Hanabata;A. Harding;M. Hayashida;R. Hughes;M. Jackson;M. Jackson;G. Jóhannesson;A. Johnson;T. Johnson;T. Johnson;W. Johnson;T. Kamae;H. Katagiri;J. Kataoka;J. Kataoka;N. Kawai;M. Kerr;J. Knödlseder;M. Kocian;M. Kuss;J. Lande;L. Latronico;S. Lee;M. Lemoine-Goumard;M. Lemoine-Goumard;F. Longo;F. Longo;F. Loparco;F. Loparco;B. Lott;B. Lott;M. Lovellette;P. Lubrano;P. Lubrano;G. Madejski;A. Makeev;A. Makeev;M. Mazziotta;C. Meurer;P. Michelson;W. Mitthumsiri;A. Moiseev;A. Moiseev;C. Monte;C. Monte;M. Monzani;A. Morselli;I. Moskalenko;S. Murgia;T. Nakamori;P. Nolan;J. Norris;E. Nuss;T. Ohsugi;E. Orlando;J. Ormes;M. Ozaki;D. Paneque;J. Panetta;D. Parent;D. Parent;V. Pelassa;M. Pepe;M. Pepe;M. Pesce-Rollins;F. Piron;T. Porter;S. Rainò;S. Rainò;R. Rando;R. Rando;M. Razzano;A. Reimer;O. Reimer;T. Reposeur;T. Reposeur;L. Rochester;A. Rodríguez;R. Romani;M. Roth;F. Ryde;H. Sadrozinski;D. Sanchez;A. Sander;P. Parkinson;J. Scargle;C. Sgro’;E. Siskind;D. Smith;D. Smith;P. Smith;G. Spandre;P. Spinelli;P. Spinelli;M. Strickman;A. Strong;D. Suson;H. Tajima;H. Takahashi;Tadayuki Takahashi;Takaaki Tanaka;J. Thayer;J. Thayer;D. Thompson;L. Tibaldo;L. Tibaldo;L. Tibaldo;D. Torres;G. Tosti;G. Tosti;A. Tramacere;Y. Uchiyama;T. Usher;A. V. Etten;V. Vasileiou;V. Vasileiou;C. Venter;C. Venter;N. Vilchez;V. Vitale;A. Waite;Pengfei Wang;B. Winer;K. Wood;T. Ylinen;M. Ziegler
通讯作者：
A. Abdo;A. Abdo;A. Abdo;M. Ackermann;M. Ajello;L. Baldini;J. Ballet;G. Barbiellini;G. Barbiellini;D. Bastieri;D. Bastieri;B. Baughman;K. Bechtol;R. Bellazzini;B. Berenji;R. Blandford;E. Bloom;E. Bonamente;E. Bonamente;A. Borgland;J. Bregeon;A. Brez;M. Brigida;M. Brigida;P. Bruel;T. Burnett;S. Buson;G. Caliandro;G. Caliandro;R. Cameron;P. Caraveo;J. Casandjian;C. Cecchi;C. Cecchi;O. Celik;O. Celik;A. Chekhtman;A. Chekhtman;C. C. Cheung-C.;J. Chiang;A. Cillis;S. Ciprini;S. Ciprini;R. Claus;J. Cohen-Tanugi;L. Cominsky;J. Conrad;J. Conrad;S. Cutini;C. Dermer;A. Angelis;F. Palma;F. Palma;E. Silva;P. Drell;A. Drlica-Wagner;R. Dubois;D. Dumora;D. Dumora;C. Farnier;C. Favuzzi;C. Favuzzi;S. Fegan;W. Focke;P. Fortin;M. Frailis;Y. Fukazawa;S. Funk;P. Fusco;P. Fusco;F. Gargano;D. Gasparrini;N. Gehrels;N. Gehrels;S. Germani;S. Germani;G. Giavitto;B. Giebels;N. Giglietto;N. Giglietto;F. Giordano;F. Giordano;T. Glanzman;G. Godfrey;I. Grenier;M. Grondin;M. Grondin;J. Grove;L. Guillemot;L. Guillemot;S. Guiriec;Y. Hanabata;A. Harding;M. Hayashida;R. Hughes;M. Jackson;M. Jackson;G. Jóhannesson;A. Johnson;T. Johnson;T. Johnson;W. Johnson;T. Kamae;H. Katagiri;J. Kataoka;J. Kataoka;N. Kawai;M. Kerr;J. Knödlseder;M. Kocian;M. Kuss;J. Lande;L. Latronico;S. Lee;M. Lemoine-Goumard;M. Lemoine-Goumard;F. Longo;F. Longo;F. Loparco;F. Loparco;B. Lott;B. Lott;M. Lovellette;P. Lubrano;P. Lubrano;G. Madejski;A. Makeev;A. Makeev;M. Mazziotta;C. Meurer;P. Michelson;W. Mitthumsiri;A. Moiseev;A. Moiseev;C. Monte;C. Monte;M. Monzani;A. Morselli;I. Moskalenko;S. Murgia;T. Nakamori;P. Nolan;J. Norris;E. Nuss;T. Ohsugi;E. Orlando;J. Ormes;M. Ozaki;D. Paneque;J. Panetta;D. Parent;D. Parent;V. Pelassa;M. Pepe;M. Pepe;M. Pesce-Rollins;F. Piron;T. Porter;S. Rainò;S. Rainò;R. Rando;R. Rando;M. Razzano;A. Reimer;O. Reimer;T. Reposeur;T. Reposeur;L. Rochester;A. Rodríguez;R. Romani;M. Roth;F. Ryde;H. Sadrozinski;D. Sanchez;A. Sander;P. Parkinson;J. Scargle;C. Sgro’;E. Siskind;D. Smith;D. Smith;P. Smith;G. Spandre;P. Spinelli;P. Spinelli;M. Strickman;A. Strong;D. Suson;H. Tajima;H. Takahashi;Tadayuki Takahashi;Takaaki Tanaka;J. Thayer;J. Thayer;D. Thompson;L. Tibaldo;L. Tibaldo;L. Tibaldo;D. Torres;G. Tosti;G. Tosti;A. Tramacere;Y. Uchiyama;T. Usher;A. V. Etten;V. Vasileiou;V. Vasileiou;C. Venter;C. Venter;N. Vilchez;V. Vitale;A. Waite;Pengfei Wang;B. Winer;K. Wood;T. Ylinen;M. Ziegler
影响因子：
2.3
作者：
M. Sawada;K. Koyama
通讯作者：
M. Sawada;K. Koyama