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Inferring the evolution pathways and the explosion mechanism of core-collapse supernova through nebular spectroscopy

FANG, Qiliang 京都大学 DOI:10.14989/doctor.k24419

2023.03.23

概要

When a massive star (with zero-age main-sequence mass >8 solar mass, or M⊙) fails in its struggle with the
gravity force after the nuclear fuel in its interior is exhausted, without the support from the thermal pressure,
the iron core collapses to form a compact object (a neutron star or a black hole). The central region quickly
reaches to the density of the neutron star, then bounce back like a piston, which creates the strong shock wave
that rapidly eject the rest of the stellar material (the ejecta), leading to the catastrophic event called
core-collapse supernova (CCSN).
The duration of the collapsing process is very short, appears to be a sudden flash which is not captured from
observation until very recent (see for example Bersten et al. 2018). The physics that governs this process is a
fascinating problem that has confused astronomers for decades, but it is very difficult to be observed for its
extremely short time scale; what we are indeed observing is the hot, expelled ejecta that shines as bright as
billions solar luminosity (a typical value is ~1049 erg s-1). Powered by the decay chain of the unstable
radioactive elements generated during the explosion, the ejecta is bright enough to be observed from distant
for months to years after the explosion. The physical properties of the ejecta, including its mass, composition,
expansion velocity and configuration etc., are key ingredients toward understanding the properties of the
supernova progenitor and the explosion.
To decode the physical properties of the ejecta, it is important to understand how the photons are generated
and propagate in the ejecta. This is usually done by radiative transfer calculation, i.e., by assuming the specific
structure of the ejecta, and then calculate how the photons look like when they escape after their complicated
interaction with the ejecta material. The result of the calculation is further compared with the observation,
from which we can extract rich information of the ejecta. A complete understanding of the ejecta structure can
not only constrain the explosion mechanism, but can also reveal the progenitor stellar system, which is also an
important unsolved problem in astronomy.
This thesis focuses on stripped-envelope supernova (SESN), a subtype of CCSNe produced by massive stars
that have loss most of the hydrogen- or helium-rich layer before the explosion. We use the late phase
(“nebular”) spectroscopy, which is taken several months after the explosion, to explore the progenitor system
of these objects, and constrain the explosion mechanism by comparing the theoretical models and the recent
observations of supernovae. ...

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List of Figures

1.1. The classification of CCSNe............................................................................................................................................................2

1.2. The illustration of the topics of interest in this thesis....................................................................................................................5

1.3. The illustration of how the analysis on nebular spectra solves the topics listed in Figure 1.2...................................................6

2.1. The V-band light curves of 7 SNe IIb and 2 SNe Ib studied in this work...................................................................................13

2.2. The lighr curve fitting results..........................................................................................................................................................16

2.3. The spectra of SNe IIb/Ib at ∼200 days after the peak magnitude is reached............................................................................17

2.4. An example of the line decomposition.............................................................................................................................................18

2.5. A comparison between the results of the two fitting strategies to the Hα-like fluxes in the nebular spectra...........................19

2.6. Evolution of the luminosities of the different nebular lines...........................................................................................................20

2.7. V-band peak magnitudes vs. the luminosities of the nebular lines in logarithmic scale, at 200 days after the V-band

maximum...................................................................................................................................................................................................23

2.8. Relative gamma-ray deposition luminosities vs. the luminosities of the nebular lines in logarithmic scale, at 200 days after

the V-band maximum...............................................................................................................................................................................23

2.9. Luminosity scatter level of Hα-like structure compared with other emission lines....................................................................24

2.10. The ejecta mass versus the line ratio of [O I] to [Ca II]...............................................................................................................25

2.11. The evolution of the luminosities of nebular lines into the very late phase................................................................................27

2.12. (1) The deposited energy vs. line luminosity at different epochs; (2) The evolution of the rms of different emission lines

and the quadratic differences of the rms of the Hα-like structure and other nebular lines..............................................................29

3.1. The average spectra of different SESN subtypes obtained around 200 days after maximum light..........................................35

3.2. The correlation between early light curve width and the [O I]/[Ca II] ratio...............................................................................35

3.3. The distribution of LN/LO ([N II]/[O I]) and LO/LCa ([O I]/[Ca II]) among different SN subtypes............................................36

3S-1. An illustration of SNe of different subtypes in this work............................................................................................................42

3S-2. Examples of the line decomposition for SNe of different subtypes............................................................................................43

3S-3.Effects of line evolutions..................................................................................................................................................................43

3S-4.The distribution of the line ratios of different SNe subtypes from 104 Monte-Carlo simulations...........................................44

4.1. The nebular spectra of the Subaru/FOCAS objects......................................................................................................................53

4.2. A detailed example of observable measurement in Section 2.3....................................................................................................55

4.3. A comparison between the line width measure in this work and previous works......................................................................56

4.4. Examples of the four line profiles....................................................................................................................................................58

143

144

4.5. The fractional flux of the secondary component is plotted against the central wavelength’s separation.................................59

4.6. (a)–(d) The distributions of the [O I] profile of different SN subtypes; In panel (e), the probability for DP detection as a

function of intrinsic DP fraction for SNe Ic-BL is shown.................................................................................................................... 61

4.7. (a) The relation between the [O I]/[Ca II] ratio and the [O I] width Δλblue. (b) Cumulative fraction of the [O I]/[Ca II] ratio.

(c) Cumulative fraction of the [O I] width Δλblue...................................................................................................................................63

4.8. Matrix of AD test significance level when the [O I]/[Ca II] and [O I] width distributions of different SN subtypes are

compared...................................................................................................................................................................................................63

4.9. Upper panel: the relation between the [O I]/[Ca II] ratio and the [O I] width Δλblue; Lower panel: the residual of the

fitting..........................................................................................................................................................................................................65

4.10.The correlations between the [O I]/[Ca II] ratio and [O I] width of different line profile classes............................................65

4.11.Upper panel: the cumulative fractions of log [O I]/[Ca II] of the objects with different line profiles;Lower panel: the

fractions of line profile as functions of log [O I]/[Ca II] are plotted by different colored solid lines and different markers........67

4.12. The fitting results of the bipolar explosion models with different degrees of axisymmetry and different viewing angles

from the direction of the poles.................................................................................................................................................................69

4.13. Upper panel: the cumulative fractions of log [O I]/[Ca II] of the objects with single-peak (NC + GS) and non-single (DP +

AS) profiles; Lower panel: the same as the lower panel of Figure 4.11 but based on the classification scheme of single-peak and

non-single profiles....................................................................................................................................................................................75

4.14. Left panels: the [O I]/[Ca II] ratio and the [O I] width Δλblue vs. the spectral phase relative to the mean value of the

sample;Middle panels: the time evolution of [O I]/[Ca II] and Δλblue of individual objects;Right panels: the distributions of the

rates of change of log [O I]/[Ca II] and log Δλblue..................................................................................................................................78

4.15. The relation between log [O I]/[Ca II] and its time evolution rate.............................................................................................80

4.16. The symmetric center of the excess emission and the deviation of the measured line widths from Δλ6563 (see the main text

for definitions)..........................................................................................................................................................................................81

4.17. Upper panel: the histogram of the central wavelength offset of the narrow core with respect to the broad base;Lower

panels: alternative fits to the SNe 2000ew and 2008ax.........................................................................................................................83

4.18. The blue solid line shows the relation between the Nred/Nblue ratio of the NC objects and the vboundary;The red solid line

shows the relation between the mean phase of the NC objects and vboundary.......................................................................................84

4.B-1. Observed [O I] of the SNe IIb in the sample fitted by multi-Gaussians..................................................................................91

4.B-2. Same as Figure 4B-1, but for the SNe Ib sample.......................................................................................................................92

4.B-3. Same as Figure 4B-1, but for the SNe Ic sample........................................................................................................................93

144

145

4.B-4. Same as Figure 4B-1, but for the SNe Ic-BL and Ib/c sample................................................................................................94

4.C-1. The evolution of [O I]/[Ca II] of well-observed SNe................................................................................................................94

5.1. Upper panel: the density structures of the He stars with MZAMS = 13, 18, 23 M⊙, and the bare CO core with MZAMS = 18, 23

M⊙; Lower panel: the mass fractions of 4He, 12C, 16O and 24Mg for the helium star with MZAMS = 20 M⊙...................................98

5.2. Upper panel: the relation between the CO core mass and the MZAMS of the progenitor models; Lower panel: the relation

between the oxygen mass and the CO core mass.................................................................................................................................99

5.3. Upper panel: the 56Ni mass fraction of He20 model with different degrees of mixing;Middle panel: the 16O mass fraction of

He20 model with different degrees of mixing;Lower panel: the

O mass fraction of CO20 model with different degrees of

mixing.....................................................................................................................................................................................................101

5.4. The physical properties of the ejecta of He18 and CO18 models (labeled by different colors) with different kinetic energies

(labeled by different line styles)...........................................................................................................................................................102

5.5. The relation between the [O I]/[Ca II] of SNe IIb model spectra (Jerkstrand et al. 2015a) and the O mass of the ejecta..103

5.6. The line profile constructed for He15 and He20 models with different kinetic energies........................................................104

5.7. The relation between VO and the EK of the ejecta.......................................................................................................................105

5.8. Upper panel: The observed [O I]/[Ca II]-line width correlation;Lower panel: The relation between the CO core mass MCO

of the models and the kinetic energy required to produce the observed [O I]/[Ca II]-line width correlation.............................107

5.9. The linear regression to the model line width VO(MO, EK) as function of oxygen mass MO and kinetic energy EK..............110

5.10. Upper panel: The model [O I] width with different degrees of macroscopic mixing; Lower panel: The [O I]/[Ca II]-line

width track of models with different degrees of macroscopic mixing while the MCO-EK relation is fixed....................................112

5.11. The MCO-EK relation required to produce the observed [O I][Ca II]-line width relation for the helium star models with

different degrees of macroscopic mixing.............................................................................................................................................112

5.12. The MCO-EK relation derived from the early phase observation..............................................................................................114

6.1. The analysis of the line widths.......................................................................................................................................................121

6.2. The configuration of the axisymmetric model..............................................................................................................................122

6.3. The occurrence rates of bipolar SNe and double-peaked [Ca II] as functions of [O I]/[Ca II]...............................................123

6.S-1. A demonstration of the line width measurement procedure of [O I] (left panels) and [Ca II] (right panels)....................125

6.S-2. The synthesized [O I] (left) and [Ca II] (right) with Vmax=5000 km s-1...................................................................................127

6.S-3. The fit of the synthesized [O I] (blue) and [Ca II] (red) to the observed line profiles (black) of the objects considered as

bipolar explosion in this work...............................................................................................................................................................128

6.S-4. The fit to the [Ca II] complex (left) and [O I] (right) of SN ...

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Inferring the evolution pathways and the explosion mechanism of core-collapse supernova through nebular spectroscopy

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Inferring the evolution pathways and the explosion mechanism of core-collapse supernova through nebular spectroscopy

概要

この論文で使われている画像

関連論文

Collapse of Rotating Massive Stars Leading to Black Hole Formation and Energetic Supernovae

Binary and Fireball as Possible Origins of Fast Radio Bursts

Long-term Evolution of a Supernova Remnant Hosting a Double Neutron Star Binary

X-ray Study on Supernova Remnants Interacting with Dense Clouds

Inferring the Progenitor Mass-Kinetic Energy Relation of Stripped-envelope Core-collapse Supernovae from Nebular Spectroscopy

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