English
 
User Manual Privacy Policy Disclaimer Contact us
  Advanced SearchBrowse

Item

ITEM ACTIONSEXPORT
  The intermediate nebular phase of SN 2014J: onset of clumping as the source of recombination

Mazzali, P. A., Bikmaev, I., Sunyaev, R., Ashall, C., Prentice, S., Tanaka, M., et al. (2020). The intermediate nebular phase of SN 2014J: onset of clumping as the source of recombination. Monthly Notices of the Royal Astronomical Society, 494(2), 2809-2822. doi:10.1093/mnras/staa839.

Item is

Basic

show hide
Item Permalink: http://hdl.handle.net/21.11116/0000-0006-BCCF-E Version Permalink: http://hdl.handle.net/21.11116/0000-0006-BCD0-B
Genre: Journal Article

Files

show Files
hide Files
:
The intermediate nebular phase of SN 2014J onset of clumping as the source of recombination.pdf (Any fulltext), 2MB
 
File Permalink:
-
Name:
The intermediate nebular phase of SN 2014J onset of clumping as the source of recombination.pdf
Description:
-
Visibility:
Private
MIME-Type / Checksum:
application/pdf
Technical Metadata:
Copyright Date:
-
Copyright Info:
-
License:
-

Locators

show

Creators

show
hide
 Creators:
Mazzali, P. A.1, Author              
Bikmaev, I., Author
Sunyaev, R., Author
Ashall, C., Author
Prentice, S., Author
Tanaka, M., Author
Irtuganov, E., Author
Melnikov, S., Author
Zhuchkov, R., Author
Affiliations:
1Stellar Astrophysics, MPI for Astrophysics, Max Planck Society, ou_159882              

Content

show
hide
Free keywords: -
 Abstract: At the age of about 1 yr, the spectra of most Type Ia supernovae (SNe Ia) are dominated by strong forbidden nebular emission lines of Fe ii and Fe iii. Later observations (at about 2 yr) of the nearby SN 2011fe showed an unexpected shift of ionization to Fe i and Fe ii. Spectra of the very nearby SN Ia 2014J at an intermediate phase (1–1.5 yr) that are presented here show a progressive decline of Fe iii emission, while Fe i is not yet strong. The decrease in ionization can be explained if the degree of clumping in the ejecta increases significantly at ∼1.5 yr, at least in the Fe-dominated zone. Models suggest that clumps remain coherent after about one year, behaving like shrapnel. The high density in the clumps, combined with the decreasing heating rate, would then cause recombination. These data may witness the phase of transition from relatively smooth ejecta to the very clumpy morphology that is typical of SN remnants. The origin of the increased clumping may be the development of local magnetic fields.

Details

show
hide
Language(s):
 Dates: 2020-04-03
 Publication Status: Published online
 Pages: -
 Publishing info: -
 Table of Contents: -
 Rev. Type: Peer
 Identifiers: DOI: 10.1093/mnras/staa839
 Degree: -

Event

show

Legal Case

show

Project information

show

Source 1

show
hide
Title: Monthly Notices of the Royal Astronomical Society
  Other : Mon. Not. R. Astron. Soc.
Source Genre: Journal
 Creator(s):
Affiliations:
Publ. Info: Oxford : Oxford University Press
Pages: - Volume / Issue: 494 (2) Sequence Number: - Start / End Page: 2809 - 2822 Identifier: ISSN: 1365-8711
CoNE: https://pure.mpg.de/cone/journals/resource/1000000000024150