Table 3: Free fitting parameters for the H $_{\alpha }$ line. The wavelength difference $\Delta \lambda$ between the narrow component and the broad component is also given. The amplitude of the narrow component is fitted manually and so no error estimate is given for this value. Since the peak of the narrow line was not included in the fitting process, no error computation of the central wavelength was carried out. We estimate the error to be similar to the values found for the other Balmer lines. Especially the value for the narrow component seems to be quite accurate compared to the rest wavelength of 6562.817 Å of the line (Moore 1972).
sp $A_{\rm n}$ $A_{\rm b}$ ${\rm\sigma_{n}}$ ${\rm\sigma_{b}}$ ${\rm\lambda_{n}}$ ${\rm\lambda_{b}}$ ${\rm\Delta\lambda}$

[ 10³ electrons] [10³ electrons] [Å] [Å] [Å] [Å] [Å]

1 2150 1232 $\pm$ 2 0.40 $\pm$ 0.04 1.91 $\pm$ 0.05 6562.80 6562.81 0.01

2 1950 807 $\pm$ 1 0.41 $\pm$ 0.03 1.78 $\pm$ 0.01 6562.78 6563.30 0.52

3 1150 419 $\pm$ 1 0.40 $\pm$ 0.04 1.68 $\pm$ 0.08 6562.79 6563.65 0.86

4 350 88 $\pm$ 0.5 0.39 $\pm$ 0.04 1.59 $\pm$ 0.15 6562.79 6563.55 0.76

5 330 46 $\pm$ 0.4 0.36 $\pm$ 0.03 1.16 $\pm$ 0.16 6562.79 6563.28 0.49

6 310 31 $\pm$ 0.4 0.35 $\pm$ 0.04 1.80 6562.79 6562.85 0.06

7 510 130 $\pm$ 0.7 0.38 $\pm$ 0.04 1.62 $\pm$ 0.16 6562.82 6562.30 -0.52

8 810 319 $\pm$ 0.9 0.38 $\pm$ 0.04 1.76 $\pm$ 0.02 6562.82 6562.62 -0.20

**Table 3:** Free fitting parameters for the H $_{\alpha }$ line. The wavelength difference $\Delta \lambda$ between the narrow component and the broad component is also given. The amplitude of the narrow component is fitted manually and so no error estimate is given for this value. Since the peak of the narrow line was not included in the fitting process, no error computation of the central wavelength was carried out. We estimate the error to be similar to the values found for the other Balmer lines. Especially the value for the narrow component seems to be quite accurate compared to the rest wavelength of 6562.817 Å of the line (Moore 1972).
sp	$A_{\rm n}$	$A_{\rm b}$	${\rm\sigma_{n}}$	${\rm\sigma_{b}}$	${\rm\lambda_{n}}$	${\rm\lambda_{b}}$	${\rm\Delta\lambda}$
	[ 10³ electrons]	[10³ electrons]	[Å]	[Å]	[Å]	[Å]	[Å]
1	2150	1232 $\pm$ 2	0.40 $\pm$ 0.04	1.91 $\pm$ 0.05	6562.80	6562.81	0.01
2	1950	807 $\pm$ 1	0.41 $\pm$ 0.03	1.78 $\pm$ 0.01	6562.78	6563.30	0.52
3	1150	419 $\pm$ 1	0.40 $\pm$ 0.04	1.68 $\pm$ 0.08	6562.79	6563.65	0.86
4	350	88 $\pm$ 0.5	0.39 $\pm$ 0.04	1.59 $\pm$ 0.15	6562.79	6563.55	0.76
5	330	46 $\pm$ 0.4	0.36 $\pm$ 0.03	1.16 $\pm$ 0.16	6562.79	6563.28	0.49
6	310	31 $\pm$ 0.4	0.35 $\pm$ 0.04	1.80	6562.79	6562.85	0.06
7	510	130 $\pm$ 0.7	0.38 $\pm$ 0.04	1.62 $\pm$ 0.16	6562.82	6562.30	-0.52
8	810	319 $\pm$ 0.9	0.38 $\pm$ 0.04	1.76 $\pm$ 0.02	6562.82	6562.62	-0.20

Source LaTeX | All tables | In the text

	1 Introduction
	2 Observations and data analysis
	3 Radial and rotational velocity
	4 Line asymmetries on LHS 2034
	5 Chromosphere simulations of LHS 2034
	6 Discussion and conclusions
	References