Luminous red novae: Stellar mergers or giant eruptions?

Tutkimustuotos: Lehtiartikkelivertaisarvioitu

Tutkijat

  • A. Pastorello
  • E. Mason
  • S. Taubenberger
  • M. Fraser
  • G. Cortini
  • L. Tomasella
  • M. T. Botticella
  • N. Elias-Rosa
  • R. Kotak
  • S. J. Smartt
  • S. Benetti
  • E. Cappellaro
  • M. Turatto
  • L. Tartaglia
  • S. G. Djorgovski
  • A. J. Drake
  • F. Briganti
  • J. Brimacombe
  • F. Bufano
  • Y-Z Cai
  • S. Chen
  • E. J. Christensen
  • F. Ciabattari
  • E. Congiu
  • A. Dimai
  • C. Inserra
  • E. Kankare
  • L. Magill
  • K. Maguire
  • F. Martinelli
  • A. Morales-Garoffolo
  • P. Ochner
  • G. Pignata
  • A. Reguitti
  • J. Sollerman
  • S. Spiro
  • G. Terreran
  • D. E. Wright

Organisaatiot

  • INAF - Osservatorio Astronomico di Padova
  • INAF, Osservatorio Astronomico di Trieste
  • Max-Planck-Institut für Astrophysik
  • European Organisation for Astronomical Research in the Southern Hemisphere (ESO)
  • University College Dublin
  • INAF, Osservatorio Astronomico di Capodimonte
  • CSIC - Institute of Space Sciences
  • Institut d´Estudis Espacials de Catalunya
  • University of Turku
  • Queen's University Belfast
  • Stockholm University
  • California Institute of Technology
  • INAF, Osservatorio Astrofisico di Catania
  • University of Padova
  • INFN, Sezione di Padova
  • Guangzhou University
  • University of Arizona
  • Osservatorio Astronomico di Monte Agliale
  • Carnegie Institution for Science
  • INAF—Osservatorio Astronomico di Brera
  • Helmut Ullrich Astronomical Observatory
  • Cardiff University
  • Gemini Observatory
  • Trinity College Dublin, The University of Dublin
  • University of Cádiz
  • Universidad Andrés Bello
  • Millennium Institute of Astrophysics (MAS)
  • Northwestern University
  • University of Minnesota

Kuvaus

We present extensive datasets for a class of intermediate-luminosity optical transients known as luminous red novae. They show double-peaked light curves, with an initial rapid luminosity rise to a blue peak (at -13 to -15 mag), which is followed by a longer-duration red peak that sometimes is attenuated, resembling a plateau. The progenitors of three of them (NGC 4490-2011OT1, M 101-2015OT1, and SNhunt248), likely relatively massive blue to yellow stars, were also observed in a pre-eruptive stage when their luminosity was slowly increasing. Early spectra obtained during the first peak show a blue continuum with superposed prominent narrow Balmer lines, with P Cygni profiles. Lines of Fe II are also clearly observed, mostly in emission. During the second peak, the spectral continuum becomes much redder, H alpha is barely detected, and a forest of narrow metal lines is observed in absorption. Very late-time spectra (similar to 6 months after blue peak) show an extremely red spectral continuum, peaking in the infrared (IR) domain. H alpha is detected in pure emission at such late phases, along with broad absorption bands due to molecular overtones (such as TiO, VO). We discuss a few alternative scenarios for luminous red novae. Although major instabilities of single massive stars cannot be definitely ruled out, we favour a common envelope ejection in a close binary system, with possibly a final coalescence of the two stars. The similarity between luminous red novae and the outburst observed a few months before the explosion of the Type IIn SN 2011ht is also discussed.

Yksityiskohdat

AlkuperäiskieliEnglanti
Artikkeli75
Sivumäärä30
JulkaisuAstronomy & Astrophysics
Vuosikerta630
TilaJulkaistu - 24 syyskuuta 2019
OKM-julkaisutyyppiA1 Julkaistu artikkeli, soviteltu

ID: 37715646