J/A+A/634/A37 TURTLS Light curves of 56Ni distributions (Magee+, 2020)
Determining the 56Ni distribution of type Ia supernovae from observations
within days of explosion.
Magee M.R., Maguire K., Kotak R., Sim S.A., Gillanders J.H., Prentice S.J.,
Skillen K.
<Astron. Astrophys. 634, A37 (2020)>
=2020A&A...634A..37M 2020A&A...634A..37M (SIMBAD/NED BibCode)
ADC_Keywords: Supernovae ; Models
Keywords: supernovae: general - radiative transfer
Abstract:
Recent studies have shown how the distribution of 56Ni within the
ejected material of type Ia supernovae can have profound consequences
on the observed light curves. Observations at early times can
therefore provide important details on the explosion physics in
thermonuclear supernovae, which are poorly constrained. To this end,
we present a series of radiative transfer calculations that explore
variations in the 56Ni distribution. Our models also show the
importance of the density profile in shaping the light curve, which is
often neglected in the literature. Using our model set, we investigate
the observations that are necessary to determine the 56Ni distribution
as robustly as possible within the current model set. Additionally, we
find that this includes observations beginning at least 14 days before
B-band maximum, extending to approximately maximum light with a
relatively high (≲3 day) cadence, and in at least one blue and one
red band are required (such as B and R, or g and r). We compare a
number of well-observed type Ia supernovae that meet these criteria to
our models and find that the light curves of 70-80% of objects in our
sample are consistent with being produced solely by variations in the
56Ni distributions. The remaining supernovae show an excess of flux
at early times, indicating missing physics that is not accounted for
within our model set, such as an interaction or the presence of
short-lived radioactive isotopes. Comparing our model light curves and
spectra to observations and delayed detonation models demonstrates
that while a somewhat extended 56Ni distribution is necessary to
reproduce the observed light curve shape, this does not negatively
affect the spectra at maximum light. Investigating current explosion
models shows that observations typically require a shallower decrease
in the 56Ni mass towards the outer ejecta than is produced for
models of a given 56Ni mass. Future models that test differences in
the explosion physics and detonation criteria should be explored to
determine the conditions necessary to reproduce the 56Ni distributions
found here.
Description:
We present the colour light curves and density profiles for models
calculated with TURTLS (Magee et al. 2018). Models are calculated
for different 56Ni masses and distributions, and density profiles.
For each model, absolute magnitude model light curves in the UBVRIgri
bands are given, in addition to a description of the ejecta density
profile and 56Ni distribution.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
list.dat 88 255 List of files
lc/* . 255 Individual model light curves
dp/* . 255 Individual model density profiles
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Byte-by-byte Description of file: list.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 A2 --- --- [Ni]
3- 5 F3.1 Msun NiMass 56Ni mass (0.4, 0.6 or 0.8)
7- 8 A2 --- --- [KE]
9- 12 F4.2 --- KE Kinetic energy (0.50, 0.60, 0.65, 0.78, 1.10,
1.40, 1.68, 1.81 or 2.18)
14 A1 --- --- [P]
15- 19 F5.1 --- P Scaling parameter (3, 4.4, 9.7, 21 or 100)
21- 56 A36 --- dp Name of the file with model density profiles
in subdirectory dp
61- 88 A28 --- lc Name of the file with model light curves
in subdirectory lc
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Byte-by-byte Description of file (#): lc/*
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 12 E12.7 d Time Days since explosion
17- 29 E13.7 mag UMAG ? Absolute U band magnitude
33- 45 E13.7 mag BMAG ? Absolute B band magnitude
49- 61 E13.7 mag VMAG Absolute V band magnitude
65- 77 E13.7 mag RMAG Absolute R band magnitude
81- 93 E13.7 mag IMAG Absolute I band magnitude
97-109 E13.7 mag gMAG ? Absolute g band magnitude
110 A1 --- n_gMAG [i] i for infinity
113-125 E13.7 mag rMAG Absolute r band magnitude
129-141 E13.7 mag iMAG Absolute i band magnitude
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Byte-by-byte Description of file (#): dp/*
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 12 E12.7 --- Index Zone index
15- 26 E12.7 km/s Velocity Zone outer velocity
34- 45 E12.7 g/cm3 Density Zone density at 20s after explosion
49- 60 E12.7 --- Fraction 56Ni mass fraction at explosion
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Acknowledgements:
Mark Magee, mrmagee.astro(at)gmail.com
(End) Mark Magee [TCD, Ireland], Patricia Vannier [CDS] 22-Dec-2019