Summary p SNR - - PowerPoint PPT Presentation
H H 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
, 2019, 12/26
Collaborators:
Cf.) Shimoda & Laming 2019a, MNRAS, 485 Shimoda & Laming 2019b, MNRAS, 489
E<1017eVSNR?!E>1017eV?!
100
Ohira, Yamazaki & Terasawa (2012)
The energy spectrum of CRs
SNR 0509-67.5 (Chandra & HST)
Blue: 1.5 – 7.0 keV Green: 0.2 – 1.5 keV Red: Ha
~TeV
From Chandra archival image
E<1017eVSNR?!E>1017eV?!
100
Ohira, Yamazaki & Terasawa (2012)
The energy spectrum of CRs
CR CRSNR →
Velocity
no CR shock (z=0)
down up
shock (z=0)
precursor CR CR
Velocity down up no CR
no CR shock (z=0)
CR CR
with CR precursor Velocity down up
no CR shock (z=0)
CR CR
with CR precursor Velocity down up
, 1 p = +
u = = w w ´ = ´ w w D = D = D = ´ W
= b b = = = =
b pr = r r r = W
= » = =
r = + » r = =
=
B dr r »
= W- r ∣ w <
p = +
= w w ´ = ´ w w D = D = D = ´ W
= b b = = = =
b pr = r r r = W
= » = =
r = + » r = =
=
B dr r »
= W- r ∣ w <
w = w 3 d » = =
W- r r =
W
=
w = W
W- r r = W-
s =
w = W
= » =
=
> = =
=
=
=
=
=
=
=
w = W-
hybrid simulation (Ohira 16)
, 1 p = +
u = = w w ´ = ´ w w D = D = D = ´ W
= b b = = = =
b pr = r r r = W
= » = =
r = + » r = =
=
B dr r »
= W- r ∣ w <
p = +
= w w ´ = ´ w w D = D = D = ´ W
= b b = = = =
b pr = r r r = W
= » = =
r = + » r = =
=
B dr r »
= W- r ∣ w <
w = w 3 d » = =
W- r r =
W
=
w = W
W- r r = W-
s =
w = W
= » =
=
> = =
=
=
=
=
=
=
=
w = W-
hybrid simulation (Ohira 16)
SNR 0509-67.5 (Chandra & HST)
Blue: 1.5 – 7.0 keV Green: 0.2 – 1.5 keV Red: Ha
~TeV
From Chandra archival image
Hα Surface Brightness −8 −6 −4 −2 2 4 6 Distance from the peak [′′] precursor postshock Shock Direction
Tycho’s SNR (Lee+2010)
Photoionization?
Hα Surface Brightness −8 −6 −4 −2 2 4 6 Distance from the peak [′′] precursor postshock Shock Direction
Tycho’s SNR (Lee+2010)
Photoionization?
RESOLVED SHOCK STRUCTURE OF THE BALMER-DOMINATED FILAMENTS IN TYCHO’S SUPERNOVA REMNANT: COSMIC-RAY PRECURSOR?
Jae-Joon Lee1, John C. Raymond2, Sangwook Park1, William P. Blair3, Parviz Ghavamian4, P. F. Winkler5, and Kelly Korreck2
1 Astronomy and Astrophysics Department, Pennsylvania State University, University Park, PA 16802, USA; lee@astro.psu.edu
< < <
SNR Cygnus Loop (Katsuda+2016) Shock Direction
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SNR Cygnus Loop (Katsuda+2016) Shock Direction
SPATIALLY RESOLVED SPECTROSCOPY OF A BALMER-DOMINATED SHOCK IN THE CYGNUS LOOP: AN EXTREMELY THIN COSMIC-RAY PRECURSOR?
Satoru Katsuda1, Keiichi Maeda2,3, Yutaka Ohira4, Yoichi Yatsu5, Koji Mori6, Wako Aoki7, Kumiko Morihana8, John C. Raymond9, Parviz Ghavamian10, Jae-Joon Lee11, Jiro Shimoda4, and Ryo Yamazaki4
1 Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), 3-1-1 Yoshinodai,
< < <
SNR Cygnus Loop (Katsuda+2016) Shock Direction
SPATIALLY RESOLVED SPECTROSCOPY OF A BALMER-DOMINATED SHOCK IN THE CYGNUS LOOP: AN EXTREMELY THIN COSMIC-RAY PRECURSOR?
Satoru Katsuda1, Keiichi Maeda2,3, Yutaka Ohira4, Yoichi Yatsu5, Koji Mori6, Wako Aoki7, Kumiko Morihana8, John C. Raymond9, Parviz Ghavamian10, Jae-Joon Lee11, Jiro Shimoda4, and Ryo Yamazaki4
1 Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), 3-1-1 Yoshinodai,
shock (z=0)
fully ionized H shock
p/e shock
emits Lyβ precursor Velocity down up
shock (z=0)
fully ionized H shock
p/e shock
emits Lyβ precursor Velocity down up Lyβ
shock (z=0)
fully ionized H shock
emits Lyβ precursor Velocity down up Lyβ τLyβ ~ 1 1s → 3p Lyβ no CR
shock (z=0)
fully ionized precursor Velocity down up Lyβ τLyβ ~ 1
1s → 3p → 2s Lyβ Hα Hα
Lyβ to Hα no CR
shock (z=0)
fully ionized precursor Velocity down up Lyβ τLyβ ~ 1
1s → 3p → 2s Lyβ Hα Hα
Lyβ to Hα y
downstream Lyβ→Hα
Shock
shock (z=0)
fully ionized precursor Velocity down up Lyβ τLyβ ~ 1
1s → 3p → 2s Lyβ Hα Hα
Lyβ to Hα no CR
shock (z=0)
fully ionized precursor Velocity down up Lyβ τLyβ ~ 1
Hα
Lyβ to Hα 2.
no CR
no CR shock (z=0)
with CR CR modified shock
precursor Velocity down up
no CR shock (z=0)
with CR
p
precursor Velocity down up H + p → p + H
no CR shock (z=0)
with CR fully ionized precursor Velocity down up Lyβ H shock
emits Lyβ
no CR shock (z=0)
with CR
fully ionized precursor Velocity down up
Lyβ
downstream Lyβ→Hα
Shock
No scattering in this direction.
no CR shock (z=0)
with CR
fully ionized precursor Velocity down up
Lyβ
no CR shock (z=0)
with CR
fully ionized precursor Velocity down up
Lyβ
Shock Te0.1 Tp .
Shock Te0.1 Tp . We solve 3 cases:
Parameters: Vsh ntot,0 proton fraction χ0 Tdown Te=βTdown Pure hydrogen plasma. 4f
(SJ & Laming 19a)
Decelerated H
3pLyβ to Hα (i.e. radiative excitation) . →ok
The sign of degree indicates the polarization angle (Stokes Q).
Polarization degree Surface brightness
p p p (Sparks+ 15).
Stokes Q Stokes U
Observed Area
Stokes Q Stokes U
Observed Area
Polarization degree Surface brightness Hβ/Hα