Stark broadening of Ca iv spectral lines of astrophysical interest

Alonso‐Medina, A.; Colón, C.

doi:10.1093/mnras/stu1855

Cited by 10 publications

(2 citation statements)

References 36 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…They are also needed for the estimation of the electron collisional rate coefficients and photoionization cross-sections so as to explain various scattering phenomena (Griem & (Firm) 1974;Zeippen 1995;Orban et al 2006). The precise evaluation of line strengths is also useful for the assessment of the Stark Broadenings of spectral lines, which is pivotal for the analysis of astrophysical phenomena (Alonso-Medina & Colón 2014). Due to this fact, the determination of radiative properties of lines present in the emission spectra of stars has become of sheer importance in the astrophysical studies.…”

Section: Introductionmentioning

confidence: 99%

Spectroscopic data of Rb-isoelectronic Zr and Nb ions for astrophysical applications

Jyoti

Kaur

Arora

et al. 2022

Preprint

View full text Add to dashboard Cite

We present high-accuracy spectroscopy data of line strengths, transition probabilities and oscillator strengths for the allowed transitions among the nS 1/2 , nP 1/2,3/2 and n ′ D 3/2,5/2 states with n = 5 to 10 and n ′ = 4 to 10 of the Rb-isoelectronic Zr (Zr IV) and Nb (Nb V) ions. They can serve to analyse various astrophysical phenomena undergoing inside the heavenly bodies containing Zr and Nb elements. Since there is a lack of precise observational and calculated data for the spectroscopic properties in the above ions, their accurate determinations are of immense interest. The literature data, that are available only for a few selected low-lying transitions, have large discrepancies and they cannot be used reliably for the above purpose. After accounting for electron interactions through random phase approximation, Brückner orbitals, structural radiations and normalizations of wave functions in the relativistic many-body methods, we have evaluated the electric dipole amplitudes precisely. Combining these values with the observed wavelengths, the above transition properties and lifetimes of a number of excited states of the Zr IV and Nb V ions are determined and compared with the literature data.

show abstract

Section: Introductionmentioning

confidence: 99%

Spectroscopic data of Rb-isoelectronic Zr and Nb ions for astrophysical applications

Jyoti

Kaur

Arora

et al. 2022

Preprint

View full text Add to dashboard Cite

show abstract

“…These radiative properties are also useful in the analysis of interstellar and quasar absorption of lines, as well as the photospheric abundance of the considered element in a given star [7]. The construction of kinetic models of plasma processes and the experimental investigations in thermonuclear reactor plasma [8,9], the estimation of the electron collisional rate coefficients and photoionization cross-sections for various scattering phenomena [10][11][12], and the assessment of Stark broadening of spectral lines involving different astrophysical phenomena [13], also aspire to more precise estimation of these radiative properties.…”

Section: Introductionmentioning

confidence: 99%

Radiative Properties of Rb-Isoelectronic Technetium (Tc VII), Ruthenium (Ru VIII) and Rhodium (Rh IX) Ions for Astrophysical Applications

Jyoti

Kaur²,

Arora³

2022

Atoms

View full text Add to dashboard Cite

In this work, we present high-accuracy spectroscopic properties, such as line strengths, transition probabilities and oscillator strengths for allowed transitions among nD3/2,5/2,n′S1/2 and n′P1/2,3/2(n=4,n′=5,6) states of Rb-isoelectronic Tc (Tc VII), Ru (Ru VIII) and Rh (Rh IX) ions for their applications in the analysis of astrophysical phenomena occurring inside celestial bodies containing Tc, Ru and Rh ions. Due to the scarcity of computational data of atomic properties of these transitions, as well as considerable discrepancies within the literature about these ions, the precise determination of these properties is necessary. For this purpose, we have implemented relativistic many-body perturbation theory (RMBPT) for evaluation of the wave functions of the considered states. For better accuracy, we have accounted for electron interactions through random phase approximation, Brückner orbitals and structural radiations of wave functions in our RMBPT method for further precise evaluation of electric dipole amplitudes. Combining these values of the observed wavelengths, the above transition properties and radiative lifetimes, a number of excited states of Tc VII, Ru VIII and Rh IX ions have been calculated. For further validation of our work, we have compared our results with the data already available in the literature.

show abstract

Division B Commission 14 Working Group: Collision Processes

Peach¹,

Dimitrijević²,

Barklem³

2015

Proc. IAU

View full text Add to dashboard Cite

Since our last report (Peach & Dimitrijević 2012), a large number of new publications on the results of research in atomic and molecular collision processes and spectral line broadening have been published. Due to the limited space available, we have only included work of importance for astrophysics. Additional relevant papers, not included in this report, can be found in the databases at the web addresses provided in Section 6. Elastic and inelastic collisions between electrons, atoms, ions, and molecules are included, as well as charge transfer in collisions between heavy particles which can be very important.

show abstract

Stark broadening of Ca iv spectral lines of astrophysical interest

Cited by 10 publications

References 36 publications

Spectroscopic data of Rb-isoelectronic Zr and Nb ions for astrophysical applications

Spectroscopic data of Rb-isoelectronic Zr and Nb ions for astrophysical applications

Radiative Properties of Rb-Isoelectronic Technetium (Tc VII), Ruthenium (Ru VIII) and Rhodium (Rh IX) Ions for Astrophysical Applications

Division B Commission 14 Working Group: Collision Processes

Contact Info

Product

Resources

About