English
 
User Manual Privacy Policy Disclaimer Contact us
  Advanced SearchBrowse

Item

ITEM ACTIONSEXPORT

Released

Journal Article

Exploring the possibility of identifying hydride and hydroxyl cations of noble gas species in the Crab Nebula filament

MPS-Authors
/persons/resource/persons133043

Caselli,  Paola
Center for Astrochemical Studies at MPE, MPI for Extraterrestrial Physics, Max Planck Society;

External Ressource
No external resources are shared
Fulltext (public)
There are no public fulltexts stored in PuRe
Supplementary Material (public)
There is no public supplementary material available
Citation

Das, A., Sil, M., Bhat, B., Gorai, P., Chakrabarti, S. K., & Caselli, P. (2020). Exploring the possibility of identifying hydride and hydroxyl cations of noble gas species in the Crab Nebula filament. The Astrophysical Journal, 902(2): 131. doi:10.3847/1538-4357/abb5fe.


Cite as: http://hdl.handle.net/21.11116/0000-0007-9168-0
Abstract
The first identification of the argonium ion (ArH+) toward the Crab Nebula supernova remnant was proclaimed by Herschel in the submillimeter and far-infrared domains. Very recently, the discovery of the hydro-helium cation (HeH+) in the planetary nebula (NGC 7027) by SOFIA has been reported. The elemental abundance of neon is much higher than that of argon. However, the presence of neonium ions (NeH+) is yet to be confirmed in space. Though the hydroxyl radicals (−OH) are very abundant in both neutral and cationic forms, hydroxyl cations of such noble gases (i.e., ArOH+, NeOH+, and HeOH+) are yet to be identified in space. Here, we employ a spectral synthesis code to examine the chemical evolution of the hydride and hydroxyl cations of the various isotopes of Ar, Ne, and He in the Crab Nebula filament and calculate their line emissivity and intrinsic line surface brightness. We successfully explain the observed surface brightness of two transitions of ArH+ (617 and 1234 GHz), one transition of OH+ (971 GHz), and one transition of H2 (2.12 μm). We also explain the observed surface brightness ratios between various molecular and atomic transitions. We find that our model reproduces the overall observed features when a hydrogen number density of ~(104–106) cm−3 and a cosmic-ray ionization rate per H2 of ~(10−11–10−10) s−1 are chosen. We discuss the possibility of detecting some hydride and hydroxyl cations in the Crab and diffuse cloud environment. Some transitions of these molecules are highlighted for future astronomical detection.