Open AccessGamma‐ray sources like V407 Cygni in symbiotic stars
Author(s) -
Lü Guoliang,
Zhu Chunhua,
Wang Zhaojun,
Huo Wensheng,
Yang Yuangui
Publication year - 2011
Publication title -
monthly notices of the royal astronomical society: letters
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.067
H-Index - 122
eISSN - 1745-3933
pISSN - 1745-3925
DOI - 10.1111/j.1745-3933.2011.01021.x
Subject(s) - physics , astrophysics , white dwarf , stars , symbiotic star , astronomy , galaxy , gamma ray , orbital period , nova (rocket) , asymptotic giant branch , spectral line , emission spectrum , aeronautics , engineering
Using a simple accelerating model and an assumption that γ‐rays originate from p–p collisions for a π 0 model, we investigate γ‐ray sources like V407 Cygni in symbiotic stars. The upper limit of their occurrence rate in the Galaxy is between 0.5 and 5 yr −1 , indicating that they may be important sources of high‐energy γ‐rays. The maximum energies of the accelerated protons mainly distribute around 10 11 eV, and barely reach 10 15 eV. The novae occurring in D‐type SSs with ONe white dwarfs and long orbital periods are good candidates for γ‐ray sources. Due to a short orbital period which results in a short acceleration duration, the nova occurring in symbiotic star RS Oph cannot produce γ‐ray emission like that in V407 Cygni.