Skip to main content Accessibility help

We use cookies to distinguish you from other users and to provide you with a better experience on our websites. Close this message to accept cookies or find out how to manage your cookie settings.

Close cookie message
×
Hostname: page-component-78c5997874-4rdpn Total loading time: 0 Render date: 2024-11-17T23:18:49.780Z Has data issue: false hasContentIssue false

Consequences of High Mass Loss Rates on Wolf-Rayet Populations in Starbursts

Published online by Cambridge University Press:  10 November 2010

G. Tenorio-Tagle
By
Georges Meynet
G. Tenorio-Tagle
Affiliation:
Instituto de Astrofísica de Canarias, Tenerife
Georges Meynet
Affiliation:
Geneva Observatory, CH-1290 Sauverny, Switzerland
Get access

Summary

We discuss the effects of a change of the mass loss rates of massive stars on the outputs of population synthesis models of starbursts. We find that models with high mass loss rates well account for the observed ratios of WNL to O-type stars in starburst galaxies.

Stellar evolutionary tracks and starburst models

The stellar populations as observed after a starburst episode depend on:

  • The intensity as a function of time of the star formation rate (SFR) during the starburst. The observed properties of the starburst may also depend on the much lower SFR if this prevails between bursts of star formation. However, for very intense bursts, these “underlying” populations can be completely blurred out by the numerous new born stars.

  • The slope of the initial mass function (IMF) and the lower and upper mass limits of the stars born in the burst.

  • The time elapsed since the beginning of the burst (which we shall call here the age of the starburst).

  • Some physical ingredients of the stellar models as, for instance, the mass loss rates by stellar winds and the metallicity.

  • […]

Type
Chapter
Information
Violent Star Formation
From 30 Doradus to QSOs
 , pp. 291 - 296
Publisher: Cambridge University Press
Print publication year: 1994

Access options

Get access to the full version of this content by using one of the access options below. (Log in options will check for institutional or personal access. Content may require purchase if you do not have access.)

Save book to Kindle

To save this book to your Kindle, first ensure coreplatform@cambridge.org is added to your Approved Personal Document E-mail List under your Personal Document Settings on the Manage Your Content and Devices page of your Amazon account. Then enter the ‘name’ part of your Kindle email address below. Find out more about saving to your Kindle.

Note you can select to save to either the @free.kindle.com or @kindle.com variations. ‘@free.kindle.com’ emails are free but can only be saved to your device when it is connected to wi-fi. ‘@kindle.com’ emails can be delivered even when you are not connected to wi-fi, but note that service fees apply.

Find out more about the Kindle Personal Document Service.

Available formats
×

Save book to Dropbox

To save content items to your account, please confirm that you agree to abide by our usage policies. If this is the first time you use this feature, you will be asked to authorise Cambridge Core to connect with your account. Find out more about saving content to Dropbox.

Available formats
×

Save book to Google Drive

To save content items to your account, please confirm that you agree to abide by our usage policies. If this is the first time you use this feature, you will be asked to authorise Cambridge Core to connect with your account. Find out more about saving content to Google Drive.

Available formats
×