Stark broadening and shift of multiply ionized carbon spectral lines

Stark-broadening calculations of singly ionized carbon spectral lines

“…Moreover, the results of Srećković et al (2000) for the 2s 2 3p 2 P o –2s 2 3d 2 D multiplet are also in very good agreement with those of Blagojević et al (1999) and our own, whereas the results of Djeniže et al (1988) are twice as large as those for our calculations and the two abovementioned experiments. Since the measurements of Djeniže et al (1988) and Srećković et al (2000) originate from the same laboratory, we may neglect the article of Djeniže et al (1988). Therefore we may conclude that the experiments of Blagojević et al (1999) and Srećković et al (2000) are in excellent agreement with the theoretical results for the 2s 2 3p 2 P o –2s 2 3d 2 D multiplet.…”

“…We can see from Table 7 that the best agreement between our present theoretical values and the experimental ones is obtained using the results of Blagojević et al (1999). Moreover, the results of Srećković et al (2000) for the 2s 2 3p 2 P o –2s 2 3d 2 D multiplet are also in very good agreement with those of Blagojević et al (1999) and our own, whereas the results of Djeniže et al (1988) are twice as large as those for our calculations and the two abovementioned experiments. Since the measurements of Djeniže et al (1988) and Srećković et al (2000) originate from the same laboratory, we may neglect the article of Djeniže et al (1988).…”

“…They are in very good agreement, better than 30 per cent (which is well within error bars), with the data of Srećković et al (2000). We will also neglect the old measurements of Djeniže et al (1988), which disagree with theory and all other experiments by a factor higher than 2. We conclude that for the 2s 2 3s 2 S–2s 2 3p 2 P o multiplet, theory and recent experiments mutually confirm each other.…”

“…To give more accuracy, a few years later Platiša, Popović & Konjević (1978) used a low‐pressure pulsed arc, while Goly & Weniger (1982a,b) used a stabilized arc and investigated ultraviolet lines. The visible spectrum was covered by Djeniže et al (1988) and Perez et al (1989): both authors used a low‐pressure pulsed arc. Sarandaev & Salakhov (1995) used an impulsive capillary discharge, Blagojević et al (1999) produced plasma with a low‐pressure pulsed arc and more recently Srećković et al (2000) investigated a large spectral range using a linear low‐pressure pulsed arc.…”

Stark Broadening of Carbon and Oxygen Lines in Hot DQ White Dwarf Stars: Recent Results and Applications

“…In the context of carbon/oxygen dominated atmosphere, it is of utmost importance to have good Stark broadening damping constants in order to derive meaningful atmospheric parameters from line profiles. However, Stark damping constants for all of the hundreds of CII lines, from UV to optical, observed in Hot DQ white dwarfs are not readily available from the literature (for example, only a few lines can be found in Griem 1974, Goly and Weniger 1982, Djenize et al 1988, Blagojevic et al 1999, Sreckovic et al 2000, Mahmoudi et al 2004 and many other references, clearly insufficient for our needs). Moreover, since the first detailed analysis of Hot DQ white dwarfs presented in Dufour et al (2007Dufour et al ( , 2008 were based on low signal-to-noise ratio SDSS observations, the first generation of Hot DQ model atmosphere were built simply using the standard approximation (see Castelli 2005): γ s /N e = 10 −8 n 5 ef f where γ s is the Stark width of the line in angular frequency units and n ef f is the effective quantum number (Kurucz linelist also gives damping constants for a few CII lines, but these values are only listed for a single temperature of 10,000 K and are based on questionable approximations as well).…”