Gamma-ray diagnostics of Type Ia supernovae

Summa, Alexander; Ulyanov, A.; Kromer, M.; Boyer, S.; Roepke, F. K.; Sim, Stuart; Seitenzahl, Ivo R.; Fink, Michael; Mannheim, K.; Pakmor, Rüdiger; Ciaraldi-Schoolmann, Franco; Diehl, R.; Maeda, Keiichi; Hillebrandt, W.

doi:10.1051/0004-6361/201220972

Cited by 31 publications

(34 citation statements)

References 49 publications

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“…Horiuchi & Beacom (2010) have simulated the gamma-ray spectra and light curves of SNe Ia, out to Virgo distances, that could be obtained by the proposed ACT mission, showing that various SD models would have distinct signatures in such gamma-ray data. Summa et al (2013) have done this exercise for the proposed GRIPS and ASTRO-H missions. They show that the same two SD and DD models, compared by Röpke et al (2012) to the optical data for SN 2011fe (see Section 3.3.3, above), could be distinguished by gamma-ray data from these missions.…”

Section: Future Outlookmentioning

confidence: 99%

Observational Clues to the Progenitors of Type Ia Supernovae

Maoz

Mannucci

Nelemans

2014

Annu. Rev. Astron. Astrophys.

941

894

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Type-Ia supernovae (SNe Ia) are important distance indicators, element factories, cosmic-ray accelerators, kinetic-energy sources in galaxy evolution, and endpoints of stellar binary evolution. It has long been clear that a SN Ia must be the runaway thermonuclear explosion of a degenerate carbon-oxygen stellar core, most likely a white dwarf (WD). However, the specific progenitor systems of SNe Ia, and the processes that lead to their ignition, have not been identified. Two broad classes of progenitor binary systems have long been considered: single-degenerate (SD), in which a WD gains mass from a non-degenerate star; and doubledegenerate (DD), involving the merger of two WDs. New theoretical work has enriched these possibilities with some interesting updates and variants. We review the significant recent observational progress in addressing the progenitor problem. We consider clues that have emerged from the observed properties of the various proposed progenitor populations, from studies of their sites -pre-and post-explosion, from analysis of the explosions themselves, and from the measurement of event rates. The recent nearby and well-studied event, SN 2011fe, has been particularly revealing. The observational results are not yet conclusive, and sometimes prone to competing theoretical interpretations. Nevertheless, it appears that DD progenitors, long considered the underdog option, could be behind some, if not all, SNe Ia. We point to some directions that may lead to future progress.

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Section: Future Outlookmentioning

confidence: 99%

Observational Clues to the Progenitors of Type Ia Supernovae

Maoz

Mannucci

Nelemans

2014

Annu. Rev. Astron. Astrophys.

941

894

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“…Many γ-ray radiative-transfer codes have utilized Monte Carlo techniques to treat the radiative transfer (Pozdnyakov et al 1983;Hoeflich et al 1992;Milne et al 2004;Sim 2007;Sim & Mazzali 2008;Summa et al 2013). Another technique, used by Swartz et al (1995) and Jeffery (1998), utilizes a grey transfer approach to treat γ-ray transport.…”

Section: Introductionmentioning

confidence: 99%

Solving the γ-ray radiative transfer equation for supernovae

Wilk

Hillier

2019

Monthly Notices of the Royal Astronomical Society

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We present a new relativistic radiative-transfer code for γ-rays of energy less than 5 MeV in supernova (SN) ejecta. This code computes the opacities, the prompt emissivity (i.e. decay), and the scattering emissivity, and solves for the intensity in the co-moving frame. Because of the large expansion velocities of SN ejecta, we ignore redistribution effects associated with thermal motions. The energy deposition is calculated from the energy removed from the radiation field by scattering or photoelectric absorption. This new code yields comparable results to an independent Monte Carlo code. However, both yield non-trivial differences with the results from a pure absorption treatment of γ-ray transport. A synthetic observer's frame spectrum is also produced from the CMF intensity. At early times when the optical depth to γrays is large, the synthetic spectrum show asymmetric line profiles with redshifted absorption as seen in SN 2014J. This new code is integrated within CMFGEN and allows for an accurate and fast computation of the decay energy deposition in SN ejecta.

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“…Kasen 2010;Bloom et al 2012;Brown et al 2012), Na I D line absorption features interpreted as evidence for circumstellar material (Patat et al 2007;Sternberg et al 2011;Dilday et al 2012), gamma-ray line and continuum emission (e.g. Sim & Mazzali 2008;Maeda et al 2012;Summa et al 2013), or the chemical evolution of Mn in the Galaxy (Seitenzahl et al 2013a), to distinguish between different explosion models.…”

Section: Introductionmentioning

confidence: 99%

5.9-keV Mn K-shell X-ray luminosity from the decay of 55Fe in Type Ia supernova models

Seitenzahl¹,

Krauß²,

Diehl³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We show that the X-ray line flux of the Mn K α line at 5.9 keV from the decay of 55 Fe is a promising diagnostic to distinguish between Type Ia supernova (SN Ia) explosion models. Using radiation transport calculations, we compute the line flux for two three-dimensional explosion models: a near-Chandrasekhar mass delayed detonation and a violent merger of two (1.1 and 0.9 M ⊙ ) white dwarfs. Both models are based on solar metallicity zero-age main sequence progenitors. Due to explosive nuclear burning at higher density, the delayeddetonation model synthesises ∼3.5 times more radioactive 55 Fe than the merger model. As a result, we find that the peak Mn K α line flux of the delayed-detonation model exceeds that of the merger model by a factor of ∼4.5. Since in both models the 5.9 keV X-ray flux peaks five to six years after the explosion, a single measurement of the X-ray line emission at this time can place a constraint on the explosion physics that is complementary to those derived from earlier phase optical spectra or light curves. We perform detector simulations of current and future X-ray telescopes to investigate the possibilities of detecting the X-ray line at 5.9 keV. Of the currently existing telescopes, XMM-Newton/pn is the best instrument for close ( 1 − 2 Mpc), non-background limited SNe Ia because of its large effective area. Due to its low instrumental background, Chandra/ACIS is currently the best choice for SNe Ia at distances above ∼2 Mpc. For the delayed-detonation scenario, a line detection is feasible with Chandra up to ∼3 Mpc for an exposure time of 10 6 s. We find that it should be possible with currently existing X-ray instruments (with exposure times 5 × 10 5 s) to detect both of our models at sufficiently high S/N to distinguish between them for hypothetical events within the Local Group. The prospects for detection will be better with future missions. For example, the proposed Athena/X-IFU instrument could detect our delayed-detonation model out to a distance of ∼5 Mpc. This would make it possible to study future events occurring during its operational life at distances comparable to those of the recent supernovae SN 2011fe (∼6.4 Mpc) and SN 2014J (∼3.5 Mpc).

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Gamma-ray diagnostics of Type Ia supernovae

Cited by 31 publications

References 49 publications

Observational Clues to the Progenitors of Type Ia Supernovae

Observational Clues to the Progenitors of Type Ia Supernovae

Solving the γ-ray radiative transfer equation for supernovae

5.9-keV Mn K-shell X-ray luminosity from the decay of 55Fe in Type Ia supernova models

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