Table 1
Properties of selected well-known PWN systems in different evolutionary stages, ordered according to the system age.
System | Crab | MSH 15-52 | G21.5-0.9 | G0.9+0.1 | Vela X | G327.1-1.1 | J1825-137 | Geminga |
---|---|---|---|---|---|---|---|---|
Age (kyr) (a) | 0.94 | 1.56 | 4.85 | 5.31 | 11.3 | 18 | 21.4 | 342 |
PSR (b) | B0531+21 | B1509-58 | J1833-1034 | J1747–2809 | B0833-45 | (c) | B1823-13 | J0633+1746 |
log (Ė) (erg s−1) | 38.65 | 37.23 | 37.53 | 37.63 | 36.84 | 36.49 | 36.45 | 34.51 |
Distance (kpc) | 2 | 4.4 | 4.1 | 8.5 | 0.28 | 9 | 3.93 | 0.25 |
RSNR (pc) | ? (d) | 38.4 | 2.98 | 19.8 | 19.5 | 22 | 120 | ? |
RPWN (pc) (e) | 2.8 | 19.2 | 0.8 | 2.5 | 12.2 | 10.5 | ? | 0.01 |
v × t (pc) (f) | 0.27 | 0.45 | 1.4 | 1.5 | 3.3 | 5.2 | 6.2 | 100 |
RTeV (pc) (g) | <3 | 11 | <4 | <7 | 2.9 | 3 | 50 | 16.2 |
RX-ray (pc) | 0.24 | 10.2 | 0.8 | 4.9 | 3.08 | 13 | 9.1 | 0.15 |
Stage (h) | 1 | 1 | 1b | 1b | 2 | 2 | 2b | 3 |
Refs. | I | II | III | IV | V | VI | VII | VIII |
Notes. (a) The pulsar characteristic age is used for the age of the system, except where historical values are known. (b) Associated pulsar (PSR). Pulsar properties are taken from Manchester et al. (2005). (c) Putative pulsar candidate identified without pulsed emission detected by Temim et al. (2009). (d) Unknown quantities are marked by “?”. (e) RPWN is the size of the PWN in radio (as opposed to the radio SNR shell). (f) v × t is the pulsar kick velocity multiplied by the age of the system, where a value of 300 km s−1 is adopted for the velocity, corresponding to the average of known values (Hansen & Phinney 1997). (g) RTeV is the one sigma radius taken from Abdalla et al. (2018b) for sources within the H.E.S.S. Galactic Plane Survey (HGPS), unless a reference is provided. (h)Stage of system evolution is assigned loosely based on age, which corresponds to Fig. 1. References. I: Frail et al. (1995), Kargaltsev et al. (2015), II: Caswell et al. (1981), Du Plessis et al. (1995), Trussoni et al. (1996), Mineo et al. (2001); III: Matheson & Safi-Harb (2010), Safi-Harb et al. (2001); IV: Green (2014), Green (2017), Dubner et al. (2008), Porquet et al. (2003); V: Duncan et al. (1996), Dwarakanath (1991), Tibaldo et al. (2018); VI: Ma et al. (2016), Temim et al. (2015); VII: Stupar et al. (2008), Duvidovich et al. (2019), Pavlov et al. (2008), Uchiyama et al. (2009); VIII: Pellizzoni et al. (2011), Abeysekara et al. (2017a), Posselt et al. (2017), Caraveo et al. (2003).
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