Coronal mass ejection precursors in Sun-like stars: Flux rope modelling and coronal signatures

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Table 1.

Parameters of the different simulated cases.

Case	x_MFR	T_MFR	B_MFR	B₀	Status
C1	–0.35	1.0	38	0.63	ESC
C2	–0.27	1.0	38	0.63	ERO
C3	0.00	1.0	38	0.63	ERO

C1 $_{T}^{+}$ $Mathematical equation: $ _{T}^{+} $$	–0.35	10.0	38	0.63	ESC
C2 $_{T}^{+}$ $Mathematical equation: $ _{T}^{+} $$	–0.27	10.0	38	0.63	ERO
C3 $_{T}^{+}$ $Mathematical equation: $ _{T}^{+} $$	0.00	10.0	38	0.63	ERO

C1 $_{T}^{-}$ $Mathematical equation: $ _{T}^{-} $$	–0.35	0.1	38	0.63	COL
C2 $_{T}^{-}$ $Mathematical equation: $ _{T}^{-} $$	–0.27	0.1	38	0.63	COL
C3 $_{T}^{-}$ $Mathematical equation: $ _{T}^{-} $$	0.00	0.1	38	0.63	ERO

C1 $_{B_{BKG}}^{+}$ $Mathematical equation: $ _{B_{\mathrm{BKG}}}^{+} $$	–0.35	1.0	38	1.26	ERO
C2 $_{B_{BKG}}^{-}$ $Mathematical equation: $ _{B_{\mathrm{BKG}}}^{-} $$	–0.27	1.0	38	0.5	ESC

C2 $_{B_{MFR}}^{+}$ $Mathematical equation: $ _{B_{\mathrm{MFR}}}^{+} $$	–0.27	1.0	43	0.63	ESC

Notes. The units for MFR positions x_MFR are expressed in R_⊙, the MFR temperature T_MFR in MK, and B₀ and B_MFR in G.

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