4 Line fluxes

Total line fluxes $F_{\rm tot}$ (ergcm^-2s^-1) for the observed emission lines are given in Tables 4 to 8, along with the peak flux $F_{\rm peak}$ (ergcm^-2s^-1Å^-1) in the line plots. The peak flux can be used in conjunction with Figs. 1-18 (except for the narrow slit observations) to get intensities through the line profiles. Note that no correction for superimposed absorption lines has been made in calculating total line fluxes.

 

 

Table 4: H and SiI line fluxes

		H$_\gamma$( 4340Å)		H$_{\delta}$ ( 4101Å)		H$_\zeta$ ( 3889Å)		H$_\eta$ ( 3835Å)		SiI ( M2; 4102Å)
Star	Phase	$F_{\rm peak}$	$F_{\rm tot}$	$F_{\rm peak}$	$F_{\rm tot}$	$F_{\rm peak}$	$F_{\rm tot}$	$F_{\rm peak}$	$F_{\rm tot}$	$F_{\rm peak}$	$F_{\rm tot}$
RR Sco	0.29	8.2-12	3.2-12	1.1-11	3.7-12	5.3-12	1.6-12	4.3-12	1.5-12	8.5-13	7.2-13
	0.58	5.0-13	2.7-13	3.5-12	1.2-12	-	-	-	-	1.2-12	6.8-13
R Aql	0.01	1.4-10	8.3-11	3.5-10	1.6-10	1.2-10	5.8-11	1.0-10	5.2-11	1.9-11	1.1-11
	0.32	3.0-12	1.6-12	3.2-12	1.0-12	1.1-12	4.9-13	1.2-12	2.8-13	-	-
	0.39	1.5-12:	1.0-12:	1.9-12:	6.2-13:	-	-	-	-	-	-
R Car	-0.16	6.1-11:	2.0-11:	1.6-10:	4.7-11:	-	-	-	-	1.9-11:	6.9-12:
	-0.09	1.1-9:	7.8-10:	1.8-9:	9.7-10:	3.1-10:	1.9-10:	1.9-10:	1.2-10:	1.2-10:	5.2-11:
	0.11	6.8-10	2.7-10	1.0-9	3.7-10	5.0-10	1.9-10	4.1-10	1.6-10	4.3-11	1.2-11
	0.39	3.7-12:	2.2-12:	-	-	-	-	-	-	-	-
S Scl	0.02	7.0-11	3.7-11	3.3-10	1.4-10	8.0-11	4.1-11	5.0-11	3.5-11	1.4-11	6.8-12
R Hya	0.08	3.0-10:	1.3-10:	2.7-10:	1.0-10:	1.7-10:	6.0-11:	8.8-11:	3.0-11:	1.8-11:	6.8-12
	0.12	2.1-10:	9.1-11:	1.1-10:	4.3-11:	9.5-11:	3.4-11:	3.2-11:	1.0-11:	2.2-11:	4.9-12:
	0.21	3.2-11	1.7-11	2.2-11	8.5-12	1.3-11	4.3-12	1.2-11	5.4-12	2.4-12	9.8-13

Notes: $F_{\rm peak}$ is the peak flux in the line in ergcm^-2s^-1Å^-1. $F_{\rm tot}$ is the total flux in the line in ergcm^-2s^-1.
Numbers followed by a colon correspond to fluxes derived by normalizing to the AAVSO light curve (see text for details).

 

 

Table 5: MgI and MnI line fluxes

		MgI ( M1; 4571Å)		MgI ( M3; 3829Å)		MgI ( M3; 3832Å)		MgI ( M3; 3838Å)		MnI ( M2; 4030Å)
Star	Phase	$F_{\rm peak}$	$F_{\rm tot}$	$F_{\rm peak}$	$F_{\rm tot}$	$F_{\rm peak}$	$F_{\rm tot}$	$F_{\rm peak}$	$F_{\rm tot}$	$F_{\rm peak}$	$F_{\rm tot}$
RR Sco	0.29	1.3-12	4.5-13	-	-	-	-	-	-	-	-
	0.48	2.9-13	6.6-14	-	-	-	-	-	-	-	-
R Aql	0.01	-	-	1.1-11	2.8-12	1.4-11	3.4-12	1.1-11	2.8-12	-	-
	0.32	2.0-12	4.8-13	-	-	-	-	-	-	-	-
	0.39	2.6-12:	7.5-13:	-	-	-	-	-	-	-	-
	0.50	6.5-13	1.7-13	-	-	-	-	-	-	-	-
R Car	-0.09	-	-	3.6-11:	1.0-11:	3.4-11:	5.7-12:	1.9-11:	3.7-12:	-	-
	0.11	-	-	2.7-11	9.6-12	3.2-11	7.2-12	3.0-11	1.5-12	-	-
	0.39	1.8-11:	3.7-12:	-	-	-	-	-	-	-	-
	0.45	6.7-12:	1.5-12:	-	-	-	-	-	-	-	-
	0.57	1.0-12	3.1-13	-	-	-	-	-	-	-	-
	0.66	4.0-13	1.4-13	-	-	-	-	-	-	-	-
R Leo	0.43	6.6-12:	1.4-12:	-	-	-	-	-	-	-	-
	0.63	9.5-13	1.8-13	-	-	-	-	-	-	-	-
	1.49	7.4-12	2.0-12	-	-	-	-	-	-	8.8-13	2.6-13
S Scl	0.52	2.6-13	6.8-14	-	-	-	-	-	-	-	-
	0.58	1.5-13	4.9-14	-	-	-	-	-	-	-	-
R Hya	0.12	9.4-12:	3.2-12:	-	-	-	-	-	-	-	-
	0.21	8.4-12	3.1-12	-	-	-	-	-	-	-	-
	0.53	1.4-12:	4.7-13:	-	-	-	-	-	-	-	-

Notes: Same as Table 4.

   

 

Table 6: FeI line fluxes

		FeI ( M2; 4461Å)		FeI ( M2; 4375Å)		FeI ( M3; 4216Å)		FeI ( M42; 4307Å)		FeI ( M42; 4202Å)
Star	Phase	$F_{\rm peak}$	$F_{\rm tot}$	$F_{\rm peak}$	$F_{\rm tot}$	$F_{\rm peak}$	$F_{\rm tot}$	$F_{\rm peak}$	$F_{\rm tot}$	$F_{\rm peak}$	$F_{\rm tot}$
RR Sco	0.29	-	-	3.6-13	1.2-13	-	-	1.4-12	7.1-13	3.9-12	7.4-13
	0.48	-	-	-	-	-	-	1.3-13	4.7-14	-	-
R Aql	0.01	-	-	-	-	-	-	-	-	9.9-12	2.3-12
	0.32	-	-	-	-	-	-	9.7-13	5.0-13	2.2-12	5.1-13
	0.39	-	-	-	-	-	-	1.4-12:	5.6-13:	2.0-12:	4.3-13:
	0.50	-	-	-	-	-	-	3.5-13	1.1-13	-	-
R Car	-0.09	-	-	1.6-11:	1.6-12:	-	-	-	-	2.9-11:	6.5-12:
	0.11	-	-	2.4-11	4.4-12	-	-	-	-	4.5-11	1.0-11
	0.39	1.6-12:	2.7-13:	1.4-12:	1.7-13:	-	-	1.2-11:	5.6-12:	9.5-12:	3.5-12:
	0.45	-	-	-	-	-	-	2.1-12:	7.6-13:	1.8-12:	6.2-13:
	0.57	-	-	-	-	-	-	7.3-13	2.1-13	-	-
	0.66	-	-	-	-	-	-	2.6-13	6.6-14	-	-
R Leo	0.43	-	-	-	-	-	-	1.5-12:	2.8-13:	-	-
	0.63	-	-	-	-	-	-	4.1-13	1.0-13	-	-
	1.49	3.6-13	7.9-14	4.0-13	8.4-14	2.5-13	5.3-14	3.7-12	1.5-12	2.6-12	1.0-12
S Scl	0.02	-	-	-	-	-	-	-	-	6.5-12	1.7-12
	0.52	-	-	-	-	-	-	2.6-13	8.4-14	-	-
	0.58	-	-	-	-	-	-	1.3-13	3.9-14	-	-
R Hya	0.08	-	-	-	-	-	-	8.0-12:	3.1-12:	4.3-11:	1.1-11:
	0.12	-	-	-	-	-	-	9.8-12:	2.8-12:	1.9-11:	5.2-12:
	0.21	-	-	-	-	-	-	5.5-12	2.5-12	1.1-11	2.9-12
	0.53	-	-	-	-	-	-	2.5-12:	7.8-13:	-	-

Notes: Same as Table 4.

 

Table 7: FeI and FeII line fluxes

		FeI ( M73; 3852Å)		FeI ( M828; 4427Å)		FeII ( M38; 4583Å)
Star	Phase	$F_{\rm peak}$	$F_{\rm tot}$	$F_{\rm peak}$	$F_{\rm tot}$	$F_{\rm peak}$	$F_{\rm tot}$
RR Sco	0.29	4.8-12	1.2-12	4.2-13	9.2-14	2.3-13	4.7-14
R Aql	0.01	1.5-11	3.5-12	-	-	-	-
	0.32	3.2-12	9.7-13	-	-	-	-
R Car	-0.09	2.7-11:	3.9-12:	-	-	-	-
	0.11	1.1-10	2.9-11	-	-	-	-
	0.39	-	-	-	-	7.7-13:	5.8-13:
R Leo	1.49	-	-	4.2-13	9.1-14	2.4-13	7.3-14
S Scl	0.02	8.5-12	1.9-12	-	-	-	-
R Hya	0.08	3.6-11:	6.8-12:	-	-	-	-
	0.12	1.9-11:	4.2-12:	-	-	-	-
	0.21	8.3-12	3.7-12	-	-	-	-

$\parbox{12.2cm}{{\em Notes}: Same as Table~\ref{HSi-table}.}$

 

Table 8: [FeII] line fluxes

		[FeII]6F		[FeII]7F		[FeII]7F		[FeII]21F		[FeII]21F
		( 4457Å)		( 4359Å)		( 4287Å)		( 4276Å)		( 4243Å)
Star	Phase	$F_{\rm peak}$	$F_{\rm tot}$	$F_{\rm peak}$	$F_{\rm tot}$	$F_{\rm peak}$	$F_{\rm tot}$	$F_{\rm peak}$	$F_{\rm tot}$	$F_{\rm peak}$	$F_{\rm tot}$
R Car	0.39	-	-	1.2-12:	2.5-13:	2.7-12:	5.5-13:	-	-	-	-
R Leo	1.49	2.3-13	9.0-14	5.4-13	1.4-13	7.8-13	3.0-13	2.6-13	7.9-14	5.4-13	1.4-13

$\parbox{16.2cm}{{\em Notes}: Same as Table~\ref{HSi-table} for [Fe\,II] line flux}$

Figure 19: Left: Absolute line fluxes plotted against phase in RLeo. Note the change in scale of the phase for we plotted the fluxes of the minimum of the next cycle in the same panel. Note also that several line fluxes are coincident at phase $\phi = 1.49$ ([FeII]7F 4359Å and [FeII]21F 4243Å; FeI 4427Å and [FeII]6F 4457Å; FeI 4461Å, FeI 4375Å and [FeII]21F 4276Å). Right: Absolute line fluxes plotted against phase in RHya. Note the coincident line fluxes at phases $\phi =0.08$ (SiI and FeI 3852Å) as well as $\phi = 0.12$ (SiI and FeI 4202Å)

Figures 19-22 show the variation with phase of all fluxes measured in each star of our sample. For the Balmer lines, both the data given in this paper and the data of Fox et al. (1984) are used in the plots. The typical variation with phase can be seen best in RCar (Fig. 22), for which a separate plot is shown for the Balmer lines. The Balmer lines H$\gamma$ and H$\delta$ appear first, roughly between phases -0.4 and -0.2 (see the Fox et al. 1984 data for RCar, SScl, RRSco and RAql as well as the present data for RCar - Figs. 20, 21 and 22). The lines then strengthen rapidly, reaching maximum flux around phase -0.1. At this phase, the other Balmer lines are observed too although they tend to reach maximum flux around phase +0.1 when the amount of overlying absorption is reduced. The Balmer lines finally vanish about phase $\phi=0.4$.

Fox et al. (1984) noted that the Balmer line fluxes can vary enormously from cycle to cycle (see o Ceti in their data), with brighter maxima yielding brighter Balmer lines. A comparison of their fluxes with ours for RCar also shows this effect. The Balmer lines we observed in RCar are roughly ten times brighter than the lines observed by Fox et al: at the same time, the AAVSO light curves show that the visual maximum during our observations ( $V \sim 3.8$) was about one magnitude brighter than the maximum ( $V \sim 4.8$) during which Fox et al. made their observations.

The SiI 4102Å (M2) high excitation line appears in all stars near maximum light. The line flux is always less than in the nearby Balmer line H$\delta$. In general, the variation with phase and the phase of the peak flux is similar to that of the hydrogen lines, although the peak flux is a factor of $\sim$10 less than in the hydrogen lines. The high excitation lines of multiplet 3 of MgI (3829.32Å, 3832.35Å and 3838.29Å) appear near maximum light and were observed in RAql and RCar (Fig. 21 right panel, and Fig. 22 left panel). The flux in these lines is about a factor of 30 less than in the Balmer lines. The lines disappear at $\phi$$\sim$0.2-0.3 and are replaced by the low excitation line of MgI (M1) at 4571.10Å. The latter appears around $\phi$$\sim$0.2-0.3 and was observed in every star of our sample, disappearing finally at the late phase $\phi$$\sim$0.6. It appears exceptionally early ($\phi = 0.12$) in RHya, as already noted in Sect. 3.2.2.

The FeI lines show a rather complex variation with phase. In general, one can divide them into two groups: type A, those appearing early in the cycle ($\sim$ maximum); and type B, those appearing around $\phi$$\sim$0.3-0.4. The first group consists of 4202.03Å (M42), 3852.57Å (M73) (both high excitation lines) and the 4375.93Å (M2) (a low excitation line). Variation of flux with phase in RHya, RAql and RCar can be seen Fig. 19 right panel, Fig. 21 right panel, and Fig. 22 left panel). These lines vary less rapidly than the Balmer or SiI lines and reach their maximum at the later phase of $\phi$$\sim$0.1.

The type B FeI emission lines 4427.29Å (M828), 4461.65Å (M2), 4216.18Å (M3) and 4307.90Å (M42) appear around $\phi$$\sim$0.3-0.4 and are usually fainter than FeI emission lines discussed above. Apart from the 4307.90Å line, these emission lines are all of low excitation. As noted in Sect. 3.2.3, the 4307.90Å line has the same upper level as the 4202.03Å line of the same multiplet and its late appearance and low flux relative to the 4202.03Å line is almost certainly due to overlying absorption. However, the flux in the 4307.90Å line at late phases is usually greater than in other late emission lines of FeI 4427.29Å, 4461.65Å and 4216.18Å. Its flux and variation with phase is quite similar to the MgI 4571.10Å line.

FeII lines were observed at late phases in a number of stars. Line fluxes of the permitted FeII 4583.84Å (M38) emission line are shown for RRSco, RCar and RLeo in Figs. 21, 22 and 19 (left panels). We note that this high excitation line appears around $\phi$$\sim$0.3-0.5 and is one of the faintest lines observed. Fluxes for the forbidden lines [FeII]7F at 4359.33Å and 4287.40Å are plotted in Fig. 22 (left panel) for RCar at phase $\phi =0.39$ and in Fig. 19 (left panel) for RLeo at $\phi = 1.49$. The line flux in RCar is similar to that of the permitted FeII emission line at 4583.84Å. In RLeo, however, the forbidden line flux is $\sim$3 times higher than the permitted line flux, at least for $\phi = 1.49$ where the forbidden lines were observed. At phase $\phi = 1.49$ in RLeo, we also measured the line fluxes of the [FeII]6F and [FeII]21F emission lines. These lines are weaker than the [FeII]7F lines: their flux is comparable to the faint, late-appearing FeI lines.

It is worth noting the much higher metal emission line fluxes during the second observed minimum of RLeo. Comparing the line fluxes of MgI 4571.10Å and FeI 4307.90Å, we see that the MgI line flux is stronger by a factor of $\sim$3 in the second cycle whereas the FeI line flux is stronger by a factor of almost 10. Finally, in Fig. 23 we summarize the overall duration and flux variation with phase of emission lines in M-type Miras.