Searching for signatures of planet formation in stars with circumstellar debris discs

J. Maldonado; C. Eiroa; E. Villaver; B. Montesinos; A. Mora

doi:10.1051/0004-6361/201525764

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Volume 579 (July 2015)

A&A, 579 (2015) A20

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Table 5

Abundance sensitivities.

	HIP 23311			HIP 77408
Ion
	Δ T _eff	Δ log g	Δ ξ _t	Δ T _eff	Δ log g	Δ ξ _t
	±43	±0.11	±0.41	±25	±0.06	±0.17
	(K)	(cm s^-2)	(km s^-1)	(K)	(cm s^-2)	(km s^-1)

C I	0.06	0.03	<0.01	0.02	0.02	<0.01
O I	0.07	0.03	0.01	0.03	0.02	0.01
Na I	0.04	0.04	0.04	0.02	0.01	0.01
Mg I	0.01	0.02	0.03	0.01	0.01	0.02
Al I	0.02	0.02	0.04	0.01	<0.01	0.01
Si I	0.02	0.02	0.01	0.01	0.01	0.01
S I	0.05	0.03	<0.01	0.02	0.02	<0.01
Ca I	0.04	0.03	0.05	0.02	0.02	0.03
Sc I	0.05	0.02	0.09	0.03	<0.01	0.01
Sc II	0.01	0.04	0.06	<0.01	0.02	0.03
Ti I	0.05	0.03	0.10	0.03	<0.01	0.04
Ti II	0.01	0.04	0.06	<0.01	0.02	0.03
V I	0.06	0.02	0.09	0.03	<0.01	0.01
Cr I	0.03	0.02	0.07	0.02	0.01	0.03
Cr II	0.03	0.04	0.05	0.01	0.02	0.03
Mn I	0.02	0.03	0.07	0.02	<0.01	0.04
Co I	<0.01	0.04	0.01	0.01	0.01	<0.01
Ni I	<0.01	0.01	0.05	0.01	0.01	0.02
Cu I	0.02	0.03	0.04	<0.01	0.02	<0.01
Zn I	0.02	0.01	0.06	0.01	0.01	0.03

	HIP 113044			HIP 28767
Ion
	Δ T _eff	Δ log g	Δ ξ _t	Δ T _eff	Δ log g	Δ ξ _t
	±20	±0.05	±0.12	±25	±0.05	±0.16
	(K)	(cm s^-2)	(km s^-1)	(K)	(cm s^-2)	(km s^-1)

C I	0.01	0.01	<0.01	0.01	0.01	<0.01
O I	0.02	0.02	0.02	0.01	0.01	0.01
Na I	0.01	0.01	0.01	0.01	0.01	0.01
Mg I	0.01	0.01	0.02	0.01	0.01	0.02
Al I	0.01	<0.01	0.01	0.01	<0.01	0.01
Si I	<0.01	<0.01	0.01	0.01	<0.01	0.01
S I	0.01	0.01	0.01	0.01	0.01	0.01
Ca I	0.01	0.01	0.03	0.02	0.01	0.03
Sc I	0.02	<0.01	<0.01	0.02	<0.01	<0.01
Sc II	<0.01	0.02	0.03	<0.01	0.02	0.03
Ti I	0.02	<0.01	0.01	0.02	<0.01	0.01
Ti II	<0.01	0.02	0.03	<0.01	0.02	0.04
V I	0.02	<0.01	<0.01	0.02	<0.01	<0.01
Cr I	0.01	<0.01	0.02	0.02	<0.01	0.03
Cr II	0.01	0.02	0.04	<0.01	0.02	0.05
Mn I	0.01	<0.01	0.03	0.02	<0.01	0.03
Co I	0.02	<0.01	<0.01	0.02	<0.01	<0.01
Ni I	0.01	<0.01	0.02	0.02	<0.01	0.01
Cu I	0.01	<0.01	<0.01	0.01	<0.01	<0.01
Zn I	<0.01	<0.01	0.04	0.01	0.01	0.04

Notes. The changes in the derived abundances when each stellar parameter is perturbed by its corresponding uncertainty are given.

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