Table 3: Splitting coefficient ( $S_{\rm c}$ ) and value of the polar field ( $B_{\rm pol})$ , at the edge of the convective core for l=2 g modes corresponding to different transitions that would produce a frequency splitting of $1\%$ , for a 4 $M_\odot$ star with an age of 94 Myr.
C_2,0-C_{2, |2|} C_{2, |1|}-C_{2, |2|}

Mode P (day) $S_{\rm c}$ (G^-2) $B_{\rm pol}$ (kG) $S_{\rm c}$ (G^-2) $B_{\rm pol}$ (kG)

g₃₅² 1.497 $6.435\times 10^{-7}$ 210 $4.827\times 10^{-7}$ 242

g₃₀² 1.281 $3.422\times 10^{-7}$ 288 $2.566\times 10^{-7}$ 332

g₁₀² 1.066 $7.897\times 10^{-9}$ 1890 $5.922\times 10^{-9}$ 2180

**Table 3:** Splitting coefficient ( $S_{\rm c}$ ) and value of the polar field ( $B_{\rm pol})$ , at the edge of the convective core for l=2 g modes corresponding to different transitions that would produce a frequency splitting of $1\%$ , for a 4 $M_\odot$ star with an age of 94 Myr.
		C_2,0-C_{2, \|2\|}		C_{2, \|1\|}-C_{2, \|2\|}
Mode	P (day)	$S_{\rm c}$ (G^-2)	$B_{\rm pol}$ (kG)		$S_{\rm c}$ (G^-2)	$B_{\rm pol}$ (kG)
g₃₅²	1.497	$6.435\times 10^{-7}$	210		$4.827\times 10^{-7}$	242
g₃₀²	1.281	$3.422\times 10^{-7}$	288		$2.566\times 10^{-7}$	332
g₁₀²	1.066	$7.897\times 10^{-9}$	1890		$5.922\times 10^{-9}$	2180

Source LaTeX | All tables | In the text

	1 Introduction
	2 Magnetic frequency splitting of g modes
	3 Model
	4 Discussion
	References