Recovery from Giant Eruptions in Very Massive Stars

Abstract

We use a hydro-and-radiative-transfer code to explore the behavior of a very massive star (VMS) after a giant eruption -- i.e., following a supernova impostor event. Beginning with reasonable models for evolved VMSs with masses of $80M_{\odot }$ and $120M_{\odot }$, we simulate the change of state caused by a giant eruption via two methods that explicitly conserve total energy: 1. Synthetically removing outer layers of mass of a few $M_{\odot }$ while reducing the energy of the inner layers. 2. Synthetically transferring energy from the core to the outer layers, an operation that automatically causes mass ejection. Our focus is on the aftermath, not the poorly-understood eruption itself. Then, using a radiation-hydrodynamic code in 1D with realistic opacities and convection, the interior disequilibrium state is followed for about 200 years. Typically the star develops a $\sim 400\mathrm{km}{\mathrm{s}}^{-1}$ wind with a mass loss rate that begins around $0.1M_{\odot }\mathrm{y}{\mathrm{r}}^{-1}$ and gradually decreases. This outflow is driven by $\kappa$-mechanism radial pulsations. The 1D models have regular pulsations but 3D models will probably be more chaotic. In some cases a plateau in the mass-loss rate may persist about 200 years, while other cases are more like $\eta$ Car which lost $>10M_{\odot }$ and then had an abnormal mass loss rate for more than a century after its eruption. In our model, the post-eruption outflow carried more mass than the initial eruption. These simulations constitute a useful preliminary reconnaissance for 3D models which will be far more difficult.

arXiv commentAccepted for publication in the ApJ

References in corpus (42)

• Modules for Experiments in Stellar Astrophysics (MESA)
• Modules for Experiments in Stellar Astrophysics (MESA): Giant Planets, Oscillations, Rotation, and Massive Stars
• Modules for Experiments in Stellar Astrophysics (MESA): Binaries, Pulsations, and Explosions
• Pre-Supernova Evolution of Massive Single and Binary Stars
• Pulsational pair instability as an explanation for the most luminous supernovae
• On the role of continuum-driven eruptions in the evolution of very massive stars and Population III stars
• The Unprecedented 2012 Outburst of SN 2009ip: A Luminous Blue Variable Becomes a True Supernova
• On the progenitor of SN 2005gl and the nature of Type IIn supernovae
• Interacting Supernovae and Supernova Impostors. SN 2009ip, is this the end?
• Luminous Blue Variable eruptions and related transients: Diversity of progenitors and outburst properties
• A panchromatic view of the restless SN2009ip reveals the explosive ejection of a massive star envelope
• On the stability of very massive primordial stars
• SN 2009ip á la PESSTO: No evidence for core-collapse yet
• Massive star evolution: Luminous Blue Variables as unexpected Supernova progenitors
• Hydrogen-Poor Circumstellar Shells from Pulsational Pair-Instability Supernovae with Rapidly Rotating Progenitors
• Multi-epoch spectropolarimetry of SN 2009ip: direct evidence for aspherical circumstellar material
• Giant Outbursts of Luminous Blue Variables and the Formation of the Homunculus Nebula Around eta Carinae
• Periastron Passage Triggering of the 19th Century Eruptions of Eta Carinae
• The Rise of the Remarkable Type IIn Supernova SN 2009ip
• The Theory of Steady State Super-Eddington Winds and its Application to Novae
• Light echoes reveal an unexpectedly cool Eta Carinae during its 19th-century Great Eruption
• Clues To The Nature of SN 2009ip from Photometric and Spectroscopic Evolution to Late Times
• Explaining the supernova impostor sn 2009ip as mergerburst
• Unmasking the Supernova Impostors
• A Model for the 19th Century Eruption of Eta Carinae: CSM Interaction Like a Scaled-Down Type IIn Supernova
• The Unusual Temporal and Spectral Evolution of the Type IIn Supernova 2011ht
• A Change in the Physical State of $\eta$ Carinae?
• The Unusual Temporal and Spectral Evolution of SN2011ht. II. Peculiar Type IIn or Impostor?
• The Early Spectra of Eta Carinae 1892 to 1941 and the Onset of Its High Excitation Emission Spectrum
• Powering the Second 2012 Outburst of SN 2009ip by Repeating Binary Interaction
• The Chrysalis Opens? Photometry from the Eta Carinae HST Treasury Project, 2002-2006
• A Sea Change in Eta Carinae
• Secular Changes in Eta Carinae's Wind 1998-2011
• Eta Carinae's 2014.6 Spectroscopic Event: Clues to the Long-term Recovery from its Great Eruption
• An Indication for the Binarity of P Cygni from Its Seventeenth Century Eruption
• Gas Dynamical Simulations of the Large and Little Homunculus Nebulae of Eta Carinae
• The Great Eruption of Eta Carinae
• Triggering Eruptive Mass Ejection in Luminous Blue Variables
• Accelerating very fast gas in the supernova impostor sn 2009ip with jets from a stellar companion
• Revisiting 2D Numerical Models for the 19th century outbursts of $\eta$ Carinae
• Near-Infrared Evidence for a Sudden Temperature Increase in Eta Carinae
• On continuum driven winds from rotating stars

Cited by in corpus (13)

• The search for failed supernovae with the Large Binocular Telescope: confirmation of a disappearing star
• The 12C(a,g)16O reaction and its implications for stellar helium burning
• On Variations Of Pre-Supernova Model Properties
• Super-Eddington Stellar Winds Driven by Near-Surface Energy Deposition
• Almost Gone: SN~2008S and NGC~300 2008OT-1 are Fainter than their Progenitors
• Common envelope jets supernova (CEJSN) impostors resulting from a neutron star companion
• Grazing envelope evolution toward Type IIb supernovae
• Pre-supernova outbursts of massive stars in the presence of a neutron star companion
• Supernovae Shock Breakout/Emergence Detection Predictions for a Wide-Field X-ray Survey
• Simulating the Response of the Secondary Star of Eta Carinae to Mass Accretion at Periastron Passage
• Fast Ejecta Resulted from Jet-Wind Interaction in the Great Eruption of Eta Carinae
• The X-ray properties of Eta Carinae during its 2020 X-ray minimum
• Accretion in massive colliding wind binaries and the effect of wind momentum ratio