Universidad de Granada Digibug

Repositorio Institucional de la Universidad de Granada >
1.-Investigación >
Departamentos, Grupos de Investigación e Institutos >
Departamento de Física Teórica y del Cosmos >
DFTC - Artículos >

Please use this identifier to cite or link to this item: http://hdl.handle.net/10481/28386

Title: Shock acceleration of relativistic particles in galaxy-galaxy collisions
Authors: Lisenfeld, Ute
Völk, Heinrich J.
Issue Date: 2010
Abstract: Context. All galaxies without a radio-loud AGN follow a tight correlation between their global far-infrared (FIR) and radio synchrotron luminosities, which is believed to be ultimately the result of the formation of massive stars. Two colliding pairs of galaxies, UGC 12914/5 and UGC 813/6 deviate from this correlation and show an excess of radio emission that in both cases originates to a large extent in a gas bridge connecting the two galactic disks.
Aims. We are aiming to clarify the origin of the radio continuum emission from the bridge.
Methods. The radio synchrotron emission expected from the bridge regions is calculated, assuming that the kinetic energy liberated in the predominantly gas dynamic interaction of the respective interstellar media (ISM) has produced shock waves that efficiently accelerate nuclei and electrons to relativistic energies. We present a model for the acceleration of relativistic particles in these shocks and calculate the resulting radio emission, its spectral index and the expected high-energy γ-ray emission.
Results. We found that the nonthermal energy produced in the collision is high enough to explain the radio emission from the bridge between the two galaxies. The calculated spectral index at the present time also agrees with the observed value. The expected γ-ray emission is not detectable with present-day instruments, but might be observable with the next generation of γ-ray telescopes.
Conclusions. The deviation of these two interacting galaxy systems from the standard FIR-radio correlation is consistent with the acceleration of an additional population of electrons in large-scale shock waves resulting from the gas dynamic interaction of the two ISM. This process is not related to star formation, and therefore it is expected that the systems do not follow the FIR-radio correlation. In particular, the radio emissions of these systems do not represent an argument against the calorimeter theory. The acceleration of relativistic electrons in shocks caused by an ISM collision, in the same way as described here, is likely to take place in other systems as well, such as galaxy clusters and groups or high-redshift systems.
Sponsorship: UL acknowledges financial support from the research project AYA2007-67625-C02-02 from the Spanish Ministerio de Ciencia y Educación and from the Junta de Andalucía.
Publisher: European Southern Observatory (ESO); Springer Verlag
Keywords: Cosmic rays
UGC 129145
Radio continuum
UGC 813/6
URI: http://hdl.handle.net/10481/28386
ISSN: 0004-6361
Rights : Creative Commons Attribution-NonCommercial-NoDerivs 3.0 License
Citation: Lisenfeld, U.; Vöelk, H.J. Shock acceleration of relativistic particles in galaxy-galaxy collisions. Astronomy and Astrophysics, 524: A27 (2010). [http://hdl.handle.net/10481/28386]
Appears in Collections:DFTC - Artículos

Files in This Item:

File Description SizeFormat
Lisenfeld_Collisions.pdf350.58 kBAdobe PDFView/Open
Recommend this item

This item is licensed under a Creative Commons License
Creative Commons

Items in DSpace are protected by copyright, with all rights reserved, unless otherwise indicated.


Valid XHTML 1.0! OpenAire compliant DSpace Software Copyright © 2002-2007 MIT and Hewlett-Packard - Feedback

© Universidad de Granada