The rates of type Ia supernovae - I. Analytical formulations

By L. Greggio. 2005

217 citations recorded by the source corpus.

The aim of this paper is to provide a handy tool to compute the impact of type Ia SN (SNIa) events on the evolution of stellar systems. An effective formalism to couple the rate of SNIa explosions from a single burst of star formation and the star formation history is presented, which rests upon the definition of the realization probability of the SNIa event ($\ensuremath{A_{\rm Ia}}$) and the distribution function of the delay times ($\ensuremath{f_{\rm Ia}}$($\ensuremath{\tau}$)). It is shown that the current SNIa rate in late type galaxies constrains $\ensuremath{A_{\rm Ia}}$ to be on the order of 10 -3 (i.e. 1 SNIa every 1000 $\ensuremath{M_\odot}$ of gas turned into stars), while the comparison of the current rates in early and late type galaxies implies that $\ensuremath{f_{\rm Ia}}$ ought to be more populated at short delays. The paper presents analytical formulations for the description of the $\ensuremath{f_{\rm Ia}}$ function for the most popular models of SNIa progenitors, namely Single Degenerates (Chandrasekhar and Sub-Chandrasekhar exploders), and Double Degenerates. These formulations follow entirely from general considerations on the evolutionary behavior of stars in binary systems, modulo a schematization of the outcome of the phases of mass exchange, and compare well with the results of population synthesis codes, for the same choice of parameters. The derivation presented here offers an immediate astrophysical interpretation of the shape of the $\ensuremath{f_{\rm Ia}}$ functions, and have a built in parametrization of the key properties of the alternative candidates. The important parameters appear to be the minimum and maximum masses of the components of the binary systems giving rise to a SNIa explosions, the distribution of the primary mass and of the mass ratios in these systems, the distribution of the separations of the DD systems at their birth. The various models for the progenitors correspond to markedly different impact on the large scales; correspondingly, the model for the progenitor can be constrained by examining the relevant observations. Among these, the paper concentrates on the trend of the current SNIa rate with parent galaxy type. The recent data by Mannucci et al. (2005, A&A, 433, 807) favor the DD channel over the SD one, which tends to predict a too steep distribution function of the delay times. The SD scenario can be reconciled with the observations only if the distribution of the mass ratios in the primordial binaries is flat and the accretion efficiency onto the WD is close to 100%. The various models are characterized by different timescales for the Fe release from a single burst stellar population. In particular the delay time within which half of the SNIa events from such a population have occurred, ranges between 0.3 and 3 Gyr, for a wide variety of hypothesis on the progenitors.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/dfbccdc07e4d2774ef75500b035cf44f4f2b00bf

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Citations in the corpus

• Radiative Feedback from Massive Black Holes in Elliptical Galaxies: AGN Flaring and Central Starburst Fueled by Recycled Gas (2007, background): “Thus, here we restrict to the currently favored s ¼ 1:1 value (Greggio 2005), even though a more complicated time dependence than a simple power law seems possible (e.g., Matteucci et al. 2006; Neill et al. 2007).”
• From star clusters to dwarf galaxies: the properties of dynamically hot stellar systems (2008, background): “Matteucci & Recchi (2001) and Greggio (2005) suggest median time scales between some ten Myr and a few Gyr for the evolution of white dwarfs into SN I, depending on the initial conditions for the population.”
• Observational Clues to the Progenitors of Type Ia Supernovae (2013, background): “Similar exponential cutoffs are seen in analytic approximations of SD model DTDs (e.g., Greggio 2005).”
• Environment and self-regulation in galaxy formation (2009, background): “…abundance ratio is a useful quantity, because it quantifies the relative importance of delayed chemical enrichment from Type Ia supernovae owing to late residual star formation (e.g. Greggio & Renzini 1983; Matteucci & Greggio 1986; Matteucci 1994; Thomas, Greggio & Bender 1999; Greggio 2005).”
• The metal content of bulge field stars from FLAMES-GIRAFFE spectra - I. Stellar parameters and iron abundances (2008, background): “Other equally plausible distributions (e.g. Greggio 2005) would have given shorter r longer timescales.”
• Production of dust by massive stars at high redshift (2011, methodology): “From explosion models (e.g., Greggio and Renzini, 1983; Matteucci and Recchi, 2001; Greggio, 2005) differentdelay times are predicted.”
• SUB-CHANDRASEKHAR WHITE DWARF MERGERS AS THE PROGENITORS OF TYPE Ia SUPERNOVAE (2010, background): “The details are complex and metallicity dependent, but below we elucidate the issues with rates estimated from basic principles (for a more formal analysis, see Greggio 2005).”
• Nearby supernova rates from the Lick Observatory Supernova Search - IV. A recovery method for the delay-time distribution (2010, methodology): “For each of several SN Ia channels, Greggio (2005) calculates the DTDs that emerge when varying the values for the parameters describing the initial conditions, and the mass and separation distributions and limits of the systems that eventually explode.”
• Europium production: neutron star mergers versus core-collapse supernovae (2013, background): “Clearly, a more realistic approach would consider a distribution functionof such timescales, in analogy with SNeIa for which a distribution fr the explosion times is defined (see Greggio 2005).”
• Rates and Properties of Type Ia Supernovae as a Function of Mass and Star Formation in Their Host Galaxies (2006, background): “This “delay-time” parameterizes the distribution of times between the binary system formation and subsequent SN explosion following accretion of material from a secondary companion (e.g. Madau, Della Valle, & Panagia 1998a, see Greggio 2005 for a review of current rate model formalizations).”
• The Progenitors of Type Ia Supernovae (2008, methodology): “Our models are different from those of Greggio (2005) since we consider the scaling of the SN Ia rate with SFR, thus minimizing the effects of variations in star formation history.”
• Two populations of progenitors for type ia supernovae (2005, methodology): “For example, the theoretical models producing wide DTDs described in section 5 (Yungelson & Livio 2000; Belczynski et al. 2005; Greggio 2005) can be modified to reproduce the empirical evidence if this strong variation of the efficiency with mass is introduced in the models, boosting the “prompt”…”
• The illustris simulation: Public data release (2015, methodology): “A catalog of synthetic stellar images and integrated spectra of galaxies in Illustris-1 at z = 0, produced using the radiative transfer code SUNRISE. For complete details on this data product, see Torrey et al. (2015) where it was first described and made available.”
• Neutron Star Mergers Might Not Be the Only Source of r-process Elements in the Milky Way (2018, methodology): “The SN Ia rate is computed following the formalism of Greggio (2005).”
• Origin of multiple stellar populations in globular clusters and their helium enrichment (2008, background): “This looks quite plausible given the wide variety of distributions of SNIa delay times that theoretical models can generate (e.g. Greggio 2005).”
• Delay Time Distribution Measurement of Type Ia Supernovae by the Subaru/XMM-Newton Deep Survey and Implications for the Progenitor (2008, unknown): “This might be useful to overcome the difficulty of the SD scenario to explain SN Ia rate at tIa>∼10 Gyr (Greggio 2005).”
• Reconstructing the star formation history of the Milky Way disc(s) from chemical abundances (2014, background): “Such a ‘double degenerate’ model could provide a drawn out tail of SNIa with very long time delay (Greggio 2005).”
• Oxygen, Sodium, Magnesium and Aluminium as tracers of the Galactic Bulge Formation (2006, background): “…theα-elements are almost instantaneously recycled in the interstellar medium (ISM), while a major fraction of iron is produced by Type Ia SNe which are characterized by a broad distribution of delay times betwe n star formation and explosion (from few 107 yrs to over 1010 yrs, e.g., Greggio 2005).”
• Nearby supernova rates from the Lick Observatory Supernova Search – III. The rate–size relation, and the rates as a function of galaxy Hubble type and colour (2010, background): “Models of binary-star evolution exists that produce both bimodalities (e.g., Greggio 2005; Hachisu et al. 2008; Lipunov et al. 2010).”
• Oxygen abundances in nearby stars - Clues to the formation and evolution of the Galactic disk (2007, background): “…stars are substantially longer, the time scale for the first SN Ia events to take place is also longer, of the order of ∼109 yr, although it should be noted that the exact value for the time scale of SN Ia events is very uncertain (see, e.g., Greggio 2005 for a recent discussion on this topic).”