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A spectroscopic analysis of the Trapezium Cluster stars

Published online by Cambridge University Press:  26 May 2016

Sergio Simón-Díaz ,
Artemio Herrero  and
César Esteban
Sergio Simón-Díaz
Affiliation:
Instituto de Astrofísica de Canarias, C/Vía Láctea s/n, E-38205 La Laguna, La Laguna, España
Artemio Herrero
Affiliation:
Instituto de Astrofísica de Canarias, C/Vía Láctea s/n, E-38205 La Laguna, La Laguna, España Departamento de Astrofísica, Universidad de La Laguna, Avda. Astrofísico Francisco Sánchez, s/n, E-38071 La Laguna, España
César Esteban
Affiliation:
Instituto de Astrofísica de Canarias, C/Vía Láctea s/n, E-38205 La Laguna, La Laguna, España Departamento de Astrofísica, Universidad de La Laguna, Avda. Astrofísico Francisco Sánchez, s/n, E-38071 La Laguna, España

Abstract

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We consider the Orion Nebula (M 42) within a project aimed at studying the interaction between massive stars and their surrounding ISM. This is an H ii region ionized by θ1 Ori C, one of the four massive stars in the Trapezium Cluster. θ1 Ori C has the earliest spectral type (O7Vp) among them, emitting an ionizing flux several orders of magnitude larger than those of the other stars. We present a spectral analysis of the Trapezium Cluster stars to determine their stellar parameters. We use spectra between 4250 – 4750 Å and compare them with synthetic spectra obtained by means of an updated version of fastwind that includes an approximated treatment of metal-line blanketing.

Type
Part 4. Feedback from Massive Stars
Information
Symposium - International Astronomical Union , Volume 212: A Massive Star Odyssey: From Main Sequence to Supernova , 2003 , pp. 749 - 750
Copyright
Copyright © Astronomical Society of the Pacific 2003 

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