Insight into the occurrence of particle acceleration through the investigation of Wolf–Rayet stars using uGMRT observations

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Table 1

Selected sample of WR stars.

Source	Spectral type	$\dot{M}$ $\[\dot{M}\]$ (10⁻⁵M_⊙ yr⁻¹)	v_∞ (km s⁻¹)	T_eff (kK)	D (kpc)	P_kin (10³⁷erg s⁻¹)
WR 87	WN7h + ?	2.5 ⁽^a⁾	1400 ⁽^a⁾	44 7 ^(b)	3.0 ⁽^c⁾	1.6
WR 93	WC7 + O7 − 9?	2.0 ⁽^d⁾	2200 ⁽^d⁾	75 ⁽^d⁾	1.76 ⁽^e⁾	3.1
WR 98a	WC8 − 9vd + ?	1.6 ⁽^f⁾	1400 ⁽^f⁾	60 ⁽^d⁾	19 ⁽^g⁾	1.0
WR 106	WC9d + ?	1.6 ⁽^h⁾	1100 ⁽^h⁾	45 ^(h)	2.32 ⁽ⁱ⁾	0.6
WR 110	WN5 − 6b + ?	1.6 ⁽^j⁾	2300 ⁽^b⁾	70.8 ⁽^b⁾	1.8 ⁽^c⁾	2.7

Notes. ^(a)Hamann et al. (1995), ^(b)Hamann et al. (2006), ^(c)Crowther et al. (2023), ^(d)Crowther (2007), ^(e)Rate & Crowther (2020),^(f⁾De Becker & Raucq (2013) ^(g)Monnier et al. (1999) ^(h)Sander et al. (2019), ⁽ⁱ⁾van der Hucht (2001), ^(j)Chené et al. (2011). The spectral type was taken from the catalogue compiled by Rosslowe & Crowther (2015) in all cases. The values for the kinetic power of the winds were derived in this work.

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