Sign on

SAO/NASA ADS Astronomy Abstract Service


· Find Similar Abstracts (with default settings below)
· Full Refereed Journal Article (PDF/Postscript)
· Full Refereed Scanned Article (GIF)
· arXiv e-print (arXiv:astro-ph/9401010)
· References in the article
· Citations to the Article (42) (Citation History)
· Refereed Citations to the Article
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Radio-emitting dust in the free electron layer of spiral galaxies: Testing the disk/halo interface
Authors:
Ferrara, A.; Dettmar, R.-J.
Affiliation:
AA(Space Telescope Science Institute, Baltimore, MD, US), AB(Space Telescope Science Institute, Baltimore, MD, US)
Publication:
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 427, no. 1, p. 155-159 (ApJ Homepage)
Publication Date:
05/1994
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
Infrared Astronomy, Interstellar Extinction, Interstellar Gas, Mathematical Models, Radiation Spectra, Spiral Galaxies, Ultraviolet Radiation, Angular Velocity, Dipole Moments, Mie Scattering, Photoelectric Emission, Radiation Pressure, Radio Emission
DOI:
10.1086/174128
Bibliographic Code:
1994ApJ...427..155F

Abstract

We present a study of the radio emission from rotating, charged dust grains immersed in the ionized gas constituting the thick, H alpha-emitting disk of many spiral galaxies. Using up-to-date optical constants, the charge on the grains exposed to the diffuse galactic UV flux has been calculated. An analytical approximation for the grain charge has been derived, which is then used to obtain the grain rotation frequency. Grains are found to have substantial radio emission peaked at a cutoff frequency in the range 10-100 GHz, depending on the grain size distribution and on the efficiency of the radiative damping of the grain rotation. The dust radio emission is compared to the free-free emission from the ionized gas component; some constraints on the magnetic field strength in the observed dusty filaments are also discussed. The model can be used to test the disk/halo interface environment in spiral galaxies, to determine the amount and size distribution of dust in their ionized component, and to investigate the rotation mechanisms for the dust. Numerical estimates are given for experimental purposes.

Printing Options

Print whole paper
Print Page(s) through

Return 600 dpi PDF to Acrobat/Browser. Different resolutions (200 or 600 dpi), formats (Postscript, PDF, etc), page sizes (US Letter, European A4, etc), and compression (gzip,compress,none) can be set through the Printing Preferences



More Article Retrieval Options

HELP for Article Retrieval


Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)

  New!

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints