The geometry of intermittent and magnetospheric state changes pulsars

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Table 1.

Known and determined parameters for intermittent pulsars.

PSR	B1931+24^a	J1841−0500^c	J1832+0029^b	J1910+0517^d	J1929+1357^d
P (s)	0.814	0.913	0.534	0.308	0.867
$R = {\dot{ν}}_{ON} / {\dot{ν}}_{OFF}$ $R={\dot {\nu }}_{\mathrm { ON}}/{\dot {\nu }}_{\mathrm {OFF}}$	1.51	2.65	1.77	-	1.8
W₁₀ ( deg)	18.0±0.5^e	26.1±2.5	9.1±1.5	32.2±3	13.4±1.4
ρ_post (deg)	7.0±0.9	6.4±0.8	7.5±1.2	11.2±1.4	6.4±0.7
k_post (deg s^0.5)	6.3±0.8	6.2±0.8	5.5±0.8	6.2±0.8	5.9±0.6
α_ρ−W (deg)	$59_{- 12}^{+ 2}$ $59^{+2}_{-12}$ (or $121_{- 2}^{+ 12}$ $121_{-2}^{+12}$ )	$31_{- 6}^{+ 3}$ $31^{+3}_{-6}$ (or $149_{- 3}^{+ 6}$ $149_{-3}^{+6}$ )	$76_{- 21}^{+ 9}$ $76^{+9}_{-21}$	$38_{- 14}^{+ 6}$ $38^{+6}_{-14}$	$69_{- 23}^{+ 14}$ $69^{+14}_{-23}$
α_RVM (deg)	121 $_{- 25}^{+ 21}$ ${}^{+21}_{-25}$	155 $_{- 9}^{+ 9}$ ${}^{+9}_{-9}$	–	–	–

Notes. We list the pulse period, P, the ratio between the spin-down values for the ON and OFF states, the determined pulse width, W_10, the posterior ρ and k values, and the resulting magnetic inclination angles for both methods, α_ρ−W and α_RVM.

^(a)

Kramer et al. (2006);

^(b)

Lorimer et al. (2012);

^(c)

Camilo et al. (2012);

^(d)

Lyne et al. (2017);

^(e)

RAN23.

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