recent results in cosmic ray physics and their interpretation author: blasi, p. arxiv: 1312.1590...
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![Page 1: Recent results in cosmic ray physics and their interpretation Author: Blasi, P. arXiv: 1312.1590 reported by Zhang Xiao](https://reader033.vdocuments.net/reader033/viewer/2022051115/56649f515503460f94c73dd4/html5/thumbnails/1.jpg)
Recent results in cosmic ray physics and their interpretation
Author: Blasi, P.
arXiv: 1312.1590
reported by Zhang Xiao
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1. Introduction
2. Status of the SNR paradigm
3. Spectral breaks
4. CR acceleration in partially ionized media and Balmer line emission in SNRs
5. summary
Outline
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1. Introduction
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2. Status of the SNR paradigm
particles are accelerated at SNR with spectral index of α
E dependent diffusive propagation with
observed CRs with spectral index α + δ ~ 2.7
◆ SNR paradigm
the test particle theory of particle acceleration: α = 2
δ = 0.7 ?
anisotropy
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2. Status of the SNR paradigm
predictions of NLDSA:
1. concave-shap spectrum
2. decrease the T of downstream gas
3. CR-induced plasma instabilities
standard DSA
efficient
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2. Status of the SNR paradigm
Escaping
When, How ... ...
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◆ B-field amplification
2. Status of the SNR paradigm
Why ?
1. to explain the thin nonthermal X-ray rims in virtually all young SNRs.
2. let maximum energy close to the knee energy.
How ?
1. due to plasma related phenomena if the shock propagates in an inhomogeneous medium.
2. CR-induced magnetic field amplification
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2. Status of the SNR paradigm
◆ test of the SNR paradigm: gamma-rays emission
I) the SNR-MCs system
II) the young individual SNRs
example: RX J1713.7-3946 and Tycho
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3. Spectral breaks
Adriani, O. et al. 2011, Sci, 332, 69
PAMELA and CREAM
80GV < Ф < 232 GVα: 2.85 ± 0.015 ± 0.004
Ф > 232 GV
α: 2.67 ± 0.03 ± 0.05
80GV < Ф < 240 GV
α: 2.766 ± 0.01±0.027
Ф > 240 GV
α: 2.477±0.06±0.03
Helium
Proton
◆ Observed results
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1. both spectra have a break at rigidity ~ 230-240 GV
2. the spectrum of He is systematically harder than the p spectrum.
3. Spectral breaks
● not confirmed by AMS-02 !
● supported by the analysis of the gamma ray spectrum of gamma rays from MCs in the Gould belt.
confirmed by AMS-02
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3. Spectral breaks
1. local source Thoudam and Horandel 2012, MNRAS, 421, 1209 Thoudam and Horandel arXiv 1304.1400
2. NLDSA at FS and RS Ptuskin et al, 2013, ApJ, 763, 5
3. propagation effects I) D(E) → D(x, E) Tomassetti, T. 2012, ApJL, 752, L13 II) pre-existing turbulence + self-generated turbulence Blasi, p. et al, 2012, SPhReL, 109, 61
4. dispersion in the spectral indices Yuan et al. 2011, PhReD, 84, 043002
Interpretation:
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4. CR acceleration in partially ionized media and Balmer line emission in SNRs
collisionless shock
upstream downstream
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neutral hydrogen with low T
ionized hydrogen with low T+
neutral hydrogen with high T
T ↑
T→
+
+exchange e-
broad Balmer line
narrow Balmer line
ionized hydrogen with high T+
◆ Balmer line emission
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4. CR acceleration in partially ionized media and Balmer line emission in SNRs
collisionless shock
upstream downstream
+
+
++
++
+
+
+
++
+
+
+
+
+
+
neutral hydrogen with low T
ionized hydrogen with low T+
neutral hydrogen with high T
T ↑
T→
+
+exchange e-
broad Balmer line
narrow Balmer line
ionized hydrogen with high T+
New phenomena under the condition of efficient acceleration
1. decrease the T of the gas downstream
2. A precursor is formed upstream
narrow the broad Balmer line
broaden the narrow Balmer line
◆ Balmer line emission
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4. CR acceleration in partially ionized media and Balmer line emission in SNRs
◆ Shape of the Balmer line emission
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4. CR acceleration in partially ionized media and Balmer line emission in SNRs
collisionless shock
upstream downstream
+
+
++
++
+
+
+
++
+
+
+
+
+
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neutral return flux ! reduce Mach number
◆ Modification caused by neutral gas
intermediate Balmer line
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4. CR acceleration in partially ionized media and Balmer line emission in SNRs
◆ Example: SNR 0509-67.5
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Thank You !
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