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 1

SNR evolution of different scenarios.

SN type	M ^a	R _b,MS ^b	R _b,RSG ^c	E _ej ^d	M _ej ^e	R _{SNR, end} ^f	t _{SNR, end} ^g	v _{SNR, end} ^h	η _esc ⁱ	E _{max, end} ^j	E _CR,end ^k

SNe IIP	8 M_⊙	0.5 pc	–	1 E₅₁	6 M_⊙	10 pc	15.5 kyr	250 km s^-1	0.1	6.5 TeV	0.23 E₅₁
SNe IIP	15 M_⊙	10 pc	1 pc	1 E₅₁	12 M_⊙	10 pc	5.8 kyr	150 km s^-1	0.1	0.8 TeV	0.12 E₅₁
SNe IIL/b	20 M_⊙	18 pc	5 pc	1 E₅₁	2 M_⊙	15 pc	6.1 kyr	2140 km s^-1	0.02	34.9 TeV	0.05 E₅₁
SNe Ib/c	25 M_⊙	22 pc	–	1 E₅₁	2 M_⊙	15 pc	2.9 kyr	2470 km s^-1	0.01	16.5 TeV	0.01 E₅₁

Notes.

^(a)

Initial mass of the progenitor star.

^(b)

Size of the MS wind bubble (including the MS bubble shell). The numbers were chosen under the reasonable assumption that the pressure of the circumstellar medium is 10⁵ K cm^-3 (Chevalier 1999; Chen et al. 2013).

^(c)

Size of RSG wind bubble, corresponding to Ṁ_RSG ≈ 0.2(5) × 10^-5M_⊙/ s and v_RSG ≈ 10(15) km s^-1 for 15 M_⊙ SNe IIP (20 M_⊙ SNe IIL/b) (Chevalier 2005).

^(d)

Total SN energy. Core-collapse SNe have observed kinetic energies of typically ~ 10⁵¹ erg( E₅₁) (Smartt 2009).

^(e)

Ejecta mass of the SN. The progenitor mass is the sum of the MS wind mass loss, the RSG wind mass loss, the neutron star mass (2 M_⊙), and the SN ejecta mass, respectively.

^(f)

For the two SNe IIP scenarios, we stop the calculations when the Sedov phase is about to end (v_SNR ≪ 1000 km s^-1), the corresponding SNR radius is around 10 pc. For the SNe IIL/b and Ib/c scenarios, we calculate the SNR history until the forward shock reaches 15 pc which is the observed radius.

^(g)

Age of the SNR when it expands to R_{SNR, end}.

^(h)

Forward shock velocity of the SNR when it expands to R_{SNR, end}.

⁽ⁱ⁾

This parameter is the ratio between the energy flux from the escaping CRs and the kinetic energy flux from the upstream medium falling to the shock. This parameter is chosen by fitting the TeV spectrum of HESS J1729-345 as described in Sect. 3 and Appendix B.

^(j)

Escape energy of CRs from the SNR shock when the shock radius has reached R_{SNR, end}.

^(k)

Total escaped CR flux integrated from the SN explosion to t_{SNR, end}.

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