Simulating the environment around planet-hosting stars - I. Coronal structure

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Volume 588 (April 2016)

A&A, 588 (2016) A28

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Table 1

Planet-hosting systems and their observational properties.


Star ID	S. Type	T _eff	R _∗	M _∗	P _rot	i	Age	Activity		M_psini	a	⟨ε_Br⟩
		[K]	[R_⊙]	[M_⊙]	[days]	[°]	[Gyr]		log (L_X)	[M_♃]	[AU]	ZDI	SH-ZDI


HD 1237^a	G8V	5572	0.86	1.00	7.00	~50	~0.88	−4.38	29.02	3.37	0.49	4.65	30.77
HD 22049^b	K2V	5146	0.74	0.86	11.68	~45	~0.44	−4.47	28.22	1.55	3.39	2.32	30.66
HD 147513^c	G5V	5930	0.98	1.07	10.00	~20	~0.45	−4.64	28.92	1.21	1.32	− ^†	6.21

Notes. The values listed in Cols. 1−12 are taken from previous studies of each system and references therein: and The last two columns contain the (radial) magnetic energy density, , averaged over the visible surface of the star, and estimated from the standard ZDI and the spherical harmonics implementation (SH-ZDI).

^(a)

Naef et al. (2001), Alvarado-Gómez et al. (2015);

^(b)

Drake & Smith (1993), Hatzes et al. (2000), Benedict et al. (2006), Jeffers et al. (2014);

^(c)

Mayor et al. (2004), Hussain et al. (2016).

^(†)

As a result of the low inclination and simple field geometry, the standard ZDI reconstruction was not possible in this case (see Brown et al. 1991).

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