Partially Ionized Zone in Orion

Bibcode
1998larm.confE..71P
Peimbert, M.; Esteban, C.; Torres-Peimbert, S.
Bibliographical reference

"IX Latin American Regional IAU Meeting, "Focal Points in Latin American Astronomy", held in Tonantzintla, Mexico, Nov 9-13, 1998, Eds: Aguilar, A.; Carraminana, A.; to be printed in Revista Mexicana de Astronomia y Astrofisica Serie de Conferencias."

Advertised on:
11
1998
Number of authors
3
IAC number of authors
1
Citations
0
Refereed citations
0
Description
We report the first reliable measurement of the nebular [OI] 5577AA emission line in the Orion nebula. The use of diagnostic diagrams using the nebular [OI] and [NI] lines and the comparison with available photoionization models, indicate that the bulk of the nebular emission of the neutral ionic species in the Orion nebula is produced in regions of low to moderate electron densities (10^3 -- 10^5 cm^-3) and electron temperatures of about 10000 K. This result is in disagreement with previous results presented in favor of very high-density regions in the partially ionized zone of the Orion nebula. The absence of such high-density zones has important consequences on the conditions where the [FeII}] emission is produced.
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