Hα Hα �������� ����������� Cf.) Shimoda & Laming 2019a, MNRAS, 485 Shimoda & Laming 2019b, MNRAS, 489 ���� 1,2 Collaborators: J. M. Laming 3 ; S. Katsuda 4 1. Nagoya Univ.; 2. Tohoku Univ.; 3. Naval Research Lab.; 4. Saitama Univ. ��������� , 2019, 12/26
Summary p ��������� SNR ������ ������������ p SNR ��������������� ����������������� ��� p Hα ��������� 判別可能 �
��������������� ���� Cosmic Rays � ��������������� The energy spectrum of CRs ��������������� Ohira, Yamazaki & Terasawa (2012) ������� dF/dE ∝ E -2.7 ���� � ������� > 10 15.5 eV ���� ����� ���� , e - , p, He, … � < 10 15.5 eV SNR Origin ��� ���� 100 ����� � ��� ������� E<10 17 eV � SNR?!E>10 17 eV ��� ?! ���� � �� �� �������� � �� , �� , �������� , 2012 � ���� ����� � ��� �� �� �������� �
Supernova Remnant (SNR) X-ray: ~TeV ���������� ������������ ����� (e.g. Warren & Hughes 04). H a : ������������ ��� From Chandra archival image (e.g. Hovey+15). SNR 0509-67.5 (Chandra & HST) Blue: 1.5 – 7.0 keV Green: 0.2 – 1.5 keV Red: H a
��������������� ���� Cosmic Rays � ��������������� The energy spectrum of CRs ��������������� Ohira, Yamazaki & Terasawa (2012) ������� dF/dE ∝ E -2.7 ���� � ������� > 10 15.5 eV ���� ����� ���� , e - , p, He, … � < 10 15.5 eV SNR Origin ��� ���� 100 ����� � ��� ���� CR ������� ������� CR ��������� SNR ��������� E<10 17 eV � SNR?!E>10 17 eV ��� ?! ���� � �� ���� → ��������� �� �� �������� � �� , �� , �������� , 2012 � ���� ����� � ��� �� �� �������� �
Cosmic-Ray Modified Shock (CRMS) Velocity no CR ������ p : protons in ������� background plasma ���� CR ������� up down z shock ( z =0)
Cosmic-Ray Modified Shock (CRMS) Velocity CR ������� no CR �������� p �� ���� ����� CR �� �������� CR heated/turbulent up precursor down z shock ( z =0)
Cosmic-Ray Modified Shock (CRMS) Velocity CR �������� no CR ��������� p �������� �� shock ����� with CR CR up precursor down z shock ( z =0)
Cosmic-Ray Modified Shock (CRMS) Velocity CR �������� no CR ��������� p �������� �� shock ����� p ����� photoionization ������ with CR � (e.g. Ghavamian+00, Medina+14). CR p ��������� CRMS ������ ��� up precursor down z shock ( z =0)
= + - p = = Cosmic-Ray Modified Shock (CRMS) ´ = w ´ w w D = D = w = w - - D = ´ W w = + - , 1 = p v W - = = » W - = - r r = - ���������� b = b = = = r u ∣ » b b = = ���� SNR ���� - = < w hybrid simulation (Ohira d » = pr 3 - 16) � - r - = = - » » W - � � w w = r r > - = W s = = = - ´ = w ´ w W - = w = w D = D = w - - » = = - - D = ´ W B B - = W = p r + r W - = = » r r r dr r » - > = W - = - = - - b = b = = = r ∣ - = = - - = = b b < w = w - - = = = = = pr w � � w = - W - = = = = r - - = = - = = - = = - = = r r - = W - = = = w - - » = = B B = p r + r » r dr r » - = = � � - w w = W = =
= + - p = = Cosmic-Ray Modified Shock (CRMS) ´ = w ´ w w D = D = w = w - - D = ´ W p ��������������� w ����������������� = + - , 1 = p v W - = = » W - = SNR ����� kpc ��������� - r r = - ���������� b = b = = = r u ∣ » b b = = ��������������� ���� SNR ���� - = < w hybrid simulation (Ohira Challenging! d » = pr 3 - 16) � - r - = = - » » W - � � w w = r r > - = W s = = = - ´ = w ´ w W - = w = w D = D = w - - » = = - - D = ´ W B B - = W = p r + r W - = = » r r r dr r » - > = W - = - = - - b = b = = = r ∣ - = = - - = = b b < w = w - - = = = = = pr w � � w = - W - = = = = r - - = = - = = - = = - = = r r - = W - = = = w - - » = = B B = p r + r » r dr r » - = = � � - w w = W = =
Supernova Remnant (SNR) X-ray: ~TeV ���������� ������������ ����� (e.g. Warren & Hughes 04). H a : ������������ ��� From Chandra archival image (e.g. Hovey+15). H a ����������������� SNR 0509-67.5 (Chandra & HST) Blue: 1.5 – 7.0 keV ��� (e.g. Raymond 91 for review). Green: 0.2 – 1.5 keV Red: H a
Hα emission from upstream Tycho’s SNR (Lee+2010) H α Surface Brightness precursor postshock Photoionization? Shock Direction − 8 − 6 − 4 − 2 0 2 4 6 Distance from the peak [ ′′ ]
Hα emission from upstream Tycho’s SNR (Lee+2010) H α Surface Brightness precursor postshock Photoionization? Shock Direction RESOLVED SHOCK STRUCTURE OF THE BALMER-DOMINATED FILAMENTS IN TYCHO ’S SUPERNOVA REMNANT: COSMIC-RAY PRECURSOR? Jae-Joon Lee 1 , John C. Raymond 2 , Sangwook Park 1 , William P. Blair 3 , Parviz Ghavamian 4 , P. F. Winkler 5 , and Kelly Korreck 2 1 Astronomy and Astrophysics Department, Pennsylvania State University, University Park, PA 16802, USA; lee@astro.psu.edu − 8 − 6 − 4 − 2 0 2 4 6 Distance from the peak [ ′′ ]
Hα emission from upstream Shock Direction SNR Cygnus Loop (Katsuda+2016) < < < + -
Hα emission from upstream Shock Direction SNR Cygnus Loop (Katsuda+2016) SPATIALLY RESOLVED SPECTROSCOPY OF A BALMER-DOMINATED SHOCK IN THE CYGNUS LOOP: AN EXTREMELY THIN COSMIC-RAY PRECURSOR? Satoru Katsuda 1 , Keiichi Maeda 2,3 , Yutaka Ohira 4 , Yoichi Yatsu 5 , Koji Mori 6 , Wako Aoki 7 , Kumiko Morihana 8 , John C. Raymond 9 , Parviz Ghavamian 10 , Jae-Joon Lee 11 , Jiro Shimoda 4 , and Ryo Yamazaki 4 1 Institute of Space and Astronautical Science ( ISAS ) , Japan Aerospace Exploration Agency ( JAXA ) , 3-1-1 Yoshinodai, < < < + -
Hα emission from upstream Shock Direction SNR Cygnus Loop (Katsuda+2016) p H a ���������������� SPATIALLY RESOLVED SPECTROSCOPY OF A BALMER-DOMINATED SHOCK IN THE CYGNUS LOOP: AN EXTREMELY THIN COSMIC-RAY PRECURSOR? Satoru Katsuda 1 , Keiichi Maeda 2,3 , Yutaka Ohira 4 , Yoichi Yatsu 5 , Koji Mori 6 , Wako Aoki 7 , Kumiko Morihana 8 , ���� John C. Raymond 9 , Parviz Ghavamian 10 , Jae-Joon Lee 11 , Jiro Shimoda 4 , and Ryo Yamazaki 4 1 Institute of Space and Astronautical Science ( ISAS ) , Japan Aerospace Exploration Agency ( JAXA ) , 3-1-1 Yoshinodai, p CR ���������������� ������������ CR ����� p Hα ��������� < < < + -
Hα emission from upstream H � shock ���� Velocity no CR H ���� p H + p/e → H* + p/e emits Lyβ p/e � shock ��� ���� up precursor down fully ionized z shock ( z =0)
Hα emission from upstream H � shock ���� Velocity no CR H ���� p H + p/e → H* + p/e Lyβ emits Lyβ p/e � shock ��� ���� up precursor down fully ionized z shock ( z =0)
Hα emission from upstream H � shock ���� Velocity no CR H ���� p H + p/e → H* + p/e Lyβ 1s → 3p τ Lyβ ~ 1 emits Lyβ p/e � shock ��� Lyβ ���� up precursor down fully ionized z shock ( z =0)
Hα emission from upstream Velocity no CR H �� Hα ���� 1. Raman �� p � Lyβ to Hα �� Lyβ 1s → 3p → 2s τ Lyβ ~ 1 Pol. Hα Hα Lyβ up precursor down fully ionized z shock ( z =0)
Hα emission from upstream Velocity no CR H �� Hα ���� 1. Raman �� p � Lyβ to Hα �� Lyβ 1s → 3p → 2s τ Lyβ ~ 1 Pol. Hα Hα Lyβ y �������������� ������ up precursor down fully ionized z shock ( z =0)
Polarization angle for Lyβ→Hα � Shock ���� �� �������� Lyβ→Hα downstream Scattered H a
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