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28 March 2024
 
  » arxiv » 2005.5972

 Article overview


The Spectacular Ultraviolet Flash From the Type Ia Supernova 2019yvq
A. A. Miller ; M. R. Magee ; A. Polin ; K. Maguire ; E. Zimmerman ; Y. Yao ; J. Sollerman ; S. Schulze ; D. A. Perley ; M. Kromer ; M. Bulla ; I. Andreoni ; E. C. Bellm ; K. De ; R. Dekany ; A. Delacroix ; S. Dhawan ; C. Fremling ; A. Gal-Yam ; D. A. Goldstein ; V. Z. Golkhou ; A. Goobar ; M. J. Graham ; I. Irani ; M. M. Kasliwal ; S. Kaye ; Y.-L. Kim ; R. R. Laher ; A. A. Mahabal ; F. J. Masci ; P. E. Nugent ; E. Ofek ; E. S. Phinney ; S. J. Prentice ; R. Riddle ; M. Rigault ; B. Rusholme ; T. Schweyer ; D. L. Shupe ; M. T. Soumagnac ; R. Walters ; L. Yan ; J. Zolkower ; S. R. Kulkarni ;
Date 12 May 2020
AbstractEarly observations of Type Ia supernovae (SNe$,$Ia) provide essential clues for understanding the progenitor system that gave rise to the terminal thermonuclear explosion. We present exquisite observations of SN$,$2019yvq, the second observed SN$,$Ia, after iPTF$,$14atg, to display an early flash of emission in the ultraviolet (UV) and optical. Our analysis finds that SN$,$2019yvq was unusual, even when ignoring the initial flash, in that it was moderately underluminous for a SN$,$Ia ($M_g approx -18.5$$,$mag at peak) yet featured very high absorption velocities ($v approx 15,000$$,mathrm{km,s}^{-1}$ for Si II $lambda$6355 at peak). We find that many of the observational features of SN$,$2019yvq, aside from the flash, can be explained if the explosive yield of radioactive $^{56}$Ni is relatively low (we measure $M_{^{56}mathrm{Ni}} = 0.31 pm 0.05,M_odot$) and it and other iron-group elements are concentrated in the innermost layers of the ejecta. To explain both the UV/optical flash and peak properties of SN$,$2019yvq we consider four different models: interaction between the SN ejecta and a nondegenerate companion, extended clumps of $^{56}$Ni in the outer ejecta, a double-detonation explosion, and the violent merger of two white dwarfs. Each of these models has shortcomings when compared to the observations; it is clear additional tuning is required to better match SN$,$2019yvq. In closing, we predict that the nebular spectra of SN$,$2019yvq will feature either H or He emission, if the ejecta collided with a companion, strong [Ca II] emission, if it was a double detonation, or narrow [O I] emission, if it was due to a violent merger.
Source arXiv, 2005.5972
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