Precessing planetary magnetospheres in SiO stars? - First detection of quasi-periodic polarization fluctuations in R Leonis and V Camelopardalis

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Table 1:

Observational results.
	V Cam	R Leo
Phase of optical lightcurve⁽¹⁾	0.08	0.10
Oscillation period of circular polarization⁽²⁾	$(5.4\pm 0.1)$ h	$(6.3 \pm 0.3)$ h
False-alarm probability⁽³⁾	4%	16%
Radial velocity of maser spots⁽⁴⁾	7.5 km s^-1	4.4 km s^-1
Mean circular polarization	$-0.3\%$	$+2.0\%$
Mean magnetic flux density in maser⁽⁵⁾	$\sim$ 100 mG	$\sim$ 1 G
Peak-to-peak variation of fractional polarization	$2.8\% = 5.6~\sigma_{\rm rms}$	$3.7\% = 7.4~\sigma_{\rm rms}$
Fluctuation of magnetic field⁽⁵⁾	$\sim$ 1 G	$\sim$ 1 G

⁽¹⁾ With respect to the maximum of the optical lightcurve; ⁽²⁾ for V Cam the second harmonic of the modelled rotation period; ⁽³⁾ with respect to the null hypothesis (data are Gaussian noise); ⁽⁴⁾ with respect to the local standard of rest; ⁽⁵⁾ order-of-magnitude estimate based on the Zeeman hypothesis, and for a linewidth of 1 km s^-1. This corresponds to a maser at $3~r_{\rm J}$ and a planetary magnetic dipole field eight times stronger than Jupiter's (Wiesemeyer 2008).

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