A young supernova remnant illuminating nearby molecular clouds with cosmic rays

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Volume 591 (July 2016)

A&A, 591 (2016) A68

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Table 3

SNR evolution when SNR evolving into the MS bubble shell.

Scenarios^a

R _b,MS

E _ej

M _ej

R _{SNR, end}

t _{SNR, end}

v _{SNR, end}

n _end ^b

η _esc

E _{max, end}

E _CR,end

E _CR,sh ^c

20M_⊙ in-shell

20.5 pc

2 E₅₁

2 M_⊙

15 pc

4.9 kyr

1150 km s^-1

0.58 cm^-3

0.02

15.6 TeV

0.13 E₅₁

0.12 E₅₁

25M_⊙ in-shell

21.5 pc

2 E₅₁

2 M_⊙

15 pc

2.4 kyr

1170 km s^-1

0.35 cm^-3

0.02

6.6 TeV

0.08 E₅₁

0.07 E₅₁

Notes.

^(a)

For both scenarios, the same initial progenitor star (scenario 20 M_⊙, SNe IIL/b and scenario 25 M_⊙, SNe Ib/c) and the same RSG bubble structure as shown in Table 1 are assumed. They only differ in MS bubble shell structure and SN energy.

^(b)

The gas density in the upstream of the shock at t_{SNR, end}.

^(c)

The total CR energy trapped inside the downstream of the shock at t_{SNR, end}. Here we roughly assume that the total CR number .

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