Solar oscillations as seen in the NaI and KI absorption lines

Bibcode
1989A&A...208..297I
Isaak, G. R.; McLeod, C. P.; Palle, P. L.; van der Raay, H. B.; Roca-Cortés, T.
Bibliographical reference

Astronomy and Astrophysics (ISSN 0004-6361), vol. 208, no. 1-2, Jan. 1989, p. 297-302. Research supported by SERC and CAICYT.

Advertised on:
1
1989
Number of authors
5
IAC number of authors
3
Citations
20
Refereed citations
18
Description
Data on the solar p modes observed simultaneously in the solar NaI and KI absorption lines were obtained in 1985 by operating two independent resonant scattering spectrometers at the same site (Observatorio del Teide, Tenerife). Since the abundances of the ground state atoms of these two elements are not the same, different depths of the solar photosphere are sampled. A comparison of the data obtained is given.
Type
Refereed
Solar atmosphere
Solar oscillations
Line of sight
Solar interior

It may interest you

  • Refereed
    Calibrating the Clock of JWST
    JWST, despite not being designed to observe astrophysical phenomena that vary on rapid timescales, can be an unparalleled tool for such studies. If timing systematics can be controlled, JWST will be able to open up the subsecond infrared timescale regime. Rapid time-domain studies, such as lag measurements in accreting compact objects and solar
    Dhillon, V. S. et al.

    Advertised on:

    1
    2025
    Bibcode
    2025AJ....169...21S
    Citations
    0
  • Refereed
    Comparing metallicity correlations in nearby non-AGN and AGN-host galaxies
    The gas-phase metallicity distribution within galaxies records critical information about galactic evolution. In this work, we investigate how active galactic nuclei (AGNs) influence this distribution by measuring the two-point correlation functions of gas-phase metallicity in 95 non-AGN and 37 AGN-host galaxies from the Calar Alto Legacy Integral
    Li, Song-Lin et al.

    Advertised on:

    1
    2025
    Bibcode
    2025MNRAS.536..430L
    Citations
    1
  • Refereed
    Why do some ultra diffuse Galaxies have rich globular cluster systems?
    Some ultra diffuse galaxies (UDGs) reveal many more globular clusters (GCs) than classical dwarf galaxies of the same stellar mass. These UDGs, with a mass in their GC system ( $M_{\rm GC}$) approaching 10 per cent of their host galaxy stellar mass ( $M_{\ast }$), are also inferred to have high halo mass to stellar mass ratios ( $M_{\rm halo}/M_{
    Forbes, Duncan A. et al.

    Advertised on:

    1
    2025
    Bibcode
    2025MNRAS.536.1217F
    Citations
    0