A massive hypergiant star as the progenitor of the supernova SN 2005gl

Gal‐Yam, A.; Leonard, Douglas C.

doi:10.1038/nature07934

Cited by 306 publications

(306 citation statements)

References 23 publications

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“…Some progenitors of Type IIn SNe are known to be near the Eddington luminosity (e.g., Gal-Yam & Leonard 2009;Smith et al 2011). The high luminosity is often related to LBVs, which are known to experience the enhanced mass loss required to explain the observational properties of Type IIn SNe (e.g., Smith 2006).…”

Section: Discussionmentioning

confidence: 99%

Mass loss of massive stars near the Eddington luminosity by core neutrino emission shortly before their explosion

Moriya

2014

A&A

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We present a novel mechanism for enhancing the mass-loss rates of massive stars shortly before their explosion. The neutrino luminosities of the stellar core of massive stars increase as they get closer to the time of the core collapse. As emitted neutrinos escape freely from the core, the core mass is significantly reduced when the neutrino luminosity is high. If a star is near the Eddington luminosity when the neutrino luminosity is high, the star can exceed the Eddington luminosity because of the core neutrino mass loss. We suggest that the stellar surface mass-loss rates due to the core neutrino emission can be higher than 10 −4 M yr −1 from ∼1 year before the core collapse. The mass-loss rates can exceed 10 −2 M yr −1 ∼ 10 days before the core collapse. This mass-loss mechanism may be able to explain the enhanced mass loss observed in some supernova progenitors shortly before their explosion. Even if the star is not close enough to the Eddington luminosity to enhance the mass loss, the star can still expand because of the reduced gravitational force. This mechanism can be activated in Wolf-Rayet stars, and it can create the hydrogen-poor, as well as hydrogen-rich, dense circumstellar media observed in some supernovae.

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Section: Discussionmentioning

confidence: 99%

Mass loss of massive stars near the Eddington luminosity by core neutrino emission shortly before their explosion

Moriya

2014

A&A

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“…It is also plausible that some SNe IIn that can be described by many of the items listed above are, in fact, SNe Ia-CSM where the CSM interaction is too strong or begins too early for any hint of an underlying SN Ia to be identified. On the other hand, at least some SNe IIn are actual core-collapse events since a massive progenitor star is detected (e.g., SN 2005gl;Gal-Yam & Leonard 2009).…”

Section: Discussionmentioning

confidence: 99%

Type Ia Supernovae Strongly Interacting with Their Circumstellar Medium

Silverman¹,

Nugent

Gal‐Yam

et al. 2015

Proc. IAU

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Owing to their utility for measurements of cosmic acceleration, Type Ia supernovae (SNe Ia) are perhaps the beststudied class of SNe, yet the progenitor systems of these explosions largely remain a mystery. A rare subclass of SNe Ia shows evidence of strong interaction with their circumstellar medium (CSM), and in particular, a hydrogenrich CSM; we refer to them as SNe Ia-CSM. In the first systematic search for such systems, we have identified 16 SNe Ia-CSM, and here we present new spectra of 13 of them. Six SNe Ia-CSM have been well studied previously, three were previously known but are analyzed in depth for the first time here, and seven are new discoveries from the Palomar Transient Factory. The spectra of all SNe Ia-CSM are dominated by Hα emission (with widths of ∼2000 km s −1 ) and exhibit large Hα/Hβ intensity ratios (perhaps due to collisional excitation of hydrogen via the SN ejecta overtaking slower-moving CSM shells); moreover, they have an almost complete lack of He i emission. They also show possible evidence of dust formation through a decrease in the red wing of Hα 75-100 days past maximum brightness, and nearly all SNe Ia-CSM exhibit strong Na i D absorption from the host galaxy. The absolute magnitudes (uncorrected for host-galaxy extinction) of SNe Ia-CSM are found to be −21.3 mag M R −19 mag, and they also seem to show ultraviolet emission at early times and strong infrared emission at late times (but no detected radio or X-ray emission). Finally, the host galaxies of SNe Ia-CSM are all late-type spirals similar to the Milky Way, or dwarf irregulars like the Large Magellanic Cloud, which implies that these objects come from a relatively young stellar population. This work represents the most detailed analysis of the SN Ia-CSM class to date.

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“…For the progenitors of SN 2005gl, however, there is no information about its preexplosion variability. One may wonder if the measured magnitude in the pre-explosion image (Gal-Yam & Leonard 2009) was obtained during a giant outburst phase. During these giant outbursts, M V increases by 3 mag or more (Humphreys & Davidson 1994) and, in this case, the progenitor of SN 2005gl could have had a much lower M V ∼ −7 mag during quiescence.…”

Section: When Lbvs Are Sn Progenitors and Their Sn Typesmentioning

confidence: 99%

“…In addition, observations suggest that some massive stars can explode as SNe already during the LBV phase (e.g. Kotak & Vink 2006;Smith et al 2007;Pastorello et al 2007;Gal-Yam & Leonard 2009). Some of these progenitors likely had M ini 50 M , which is much higher than the range of LBVs that can be SN progenitors based on single stellar evolution models (20 M < ∼ M ini < ∼ 25 M ; Groh et al 2013).…”

Section: Introductionmentioning

confidence: 99%

Fundamental properties of core-collapse supernova and GRB progenitors: predicting the look of massive stars before death

Groh

Meynet

Georgy

et al. 2013

A&A

193

223

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We investigate the fundamental properties of core-collapse supernova (SN) progenitors from single stars at solar metallicity. For this purpose, we combine Geneva stellar evolutionary models with initial masses of M ini = 20−120 M with atmospheric and wind models using the radiative transfer code CMFGEN. We provide synthetic photometry and high-resolution spectra of hot stars at the pre-SN stage. For models with M ini = 9−20 M , we supplement our analysis using publicly available MARCS model atmospheres of RSGs to estimate their synthetic photometry. We employ well-established observational criteria of spectroscopic classification and find that, depending on their initial mass and rotation, massive stars end their lives as red supergiants (RSG), yellow hypergiants (YHG), luminous blue variables (LBV), and Wolf-Rayet (WR) stars of the WN and WO spectral types. For rotating models, we obtained the following types of SN progenitors:, and RSGs (9 ≤ M ini ≤ 18 M ). For non-rotating models, we found spectral types WO1-, and RSGs (9 ≤ M ini ≤ 20 M ). Our rotating models indicate that SN IIP progenitors are all RSG, SN IIL/b progenitors are 56% LBVs and 44% YHGs, SN Ib progenitors are 96% WN10-11 and 4% WOs, and SN Ic progenitors are all WO stars. We find that the most massive and luminous SN progenitors are not necessarily the brightest ones in a given filter, since this depends on their luminosity, temperature, wind density, and the way the spectral energy distribution compares to a filter bandpass. We find that SN IIP progenitors (RSGs) are bright in the RIJHK S filters and faint in the UB filters. SN IIL/b progenitors (LBVs and YHGs), and SN Ib progenitors (WNs) are relatively bright in optical/infrared filters, while SN Ic progenitors (WOs) are faint in all optical filters. We argue that SN Ib and Ic progenitors from single stars should be undetectable in the available pre-explosion images with the current magnitude limits, in agreement with observational results.

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A massive hypergiant star as the progenitor of the supernova SN 2005gl

Cited by 306 publications

References 23 publications

Mass loss of massive stars near the Eddington luminosity by core neutrino emission shortly before their explosion

Mass loss of massive stars near the Eddington luminosity by core neutrino emission shortly before their explosion

Type Ia Supernovae Strongly Interacting with Their Circumstellar Medium

Fundamental properties of core-collapse supernova and GRB progenitors: predicting the look of massive stars before death

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