Spectral Metallicity in M33

Bibcode
1997ASSL..212..207M
Monteverde, M. I.; Herrero, A.; Lennon, D. J.; Kudritzki, R. P.
Bibliographical reference

"Wide-field spectroscopy, Proceedings of the 2nd conference of the Working Group of IAU Commission 9 on "Wide-Field Imaging" held in Athens, Greece, May 20-25, 1996. Edited by E. Kontizas, M. Kontizas, D.H. Morgan, and G.P. Vettolani. Publisher: Dordrecht: Kluwer Academic Publishers, 1997, Astrophysics and Space Science Library, Vol. 212, ISBN: 0792345185, p.207"

Advertised on:
0
1997
Number of authors
4
IAC number of authors
0
Citations
0
Refereed citations
0
Description
Not Available
Type
Non-refereed

It may interest you

  • Non-refereed
    Einasto Gravitational Potentials have Difficulty to Hold Spherically Symmetric Stellar Systems with Cores
    It was known that an ideal spherically symmetric stellar system with isotropic velocities and an inner core cannot reside in a Navarro, Frenk, and White (NFW) gravitational potential. The incompatibility can be pinned down to the radial gradient of the NFW potential in the very center of the system, which differs from zero. The gradient is
    Sánchez Almeida, Jorge

    Advertised on:

    6
    2024
    Bibcode
    2024RNAAS...8..167S
    Citations
    0
  • Non-refereed
    The Aligned Orbit of a Hot Jupiter around the M Dwarf TOI-4201
    Measuring the obliquities of stars hosting giant planets may shed light on the dynamical history of planetary systems. Significant efforts have been made to measure the obliquities of FGK stars with hot Jupiters, mainly based on observations of the Rossiter–McLaughlin effect. In contrast, M dwarfs with hot Jupiters have hardly been explored because
    Gan, Tianjun et al.

    Advertised on:

    7
    2024
    Bibcode
    2024ApJ...969L..24G
  • Non-refereed
    A Systematic Search for and Characterization of White Dwarf Binaries Across the H-R Diagram
    White dwarfs (WDs) are the endpoint of evolution for 97% of stars. Most of these stars are in multiple systems, and a significant fraction of those are compact enough to exchange mass, altering the structures and subsequent evolution of both stars. The physical mechanisms that facilitate these mass exchanges include common envelope evolution, Roche
    Anguiano, Borja et al.

    Advertised on:

    6
    2024
    Bibcode
    2024AAS...24410807A
    Citations
    0