Studying explosive phenomena in astrophysics by the example of gamma-ray bursts and supernovae

124 Pages·2015·7.28 MB·English

by  Anastasia Filina

UNIVERSITE NICE SOPHIA ANTIPOLIS - UFR Sciences
EcoleDoctoraleenSciencesFondamentalesetAppliquees
THESE
pourobtenirletitrede
Docteur en Sciences
del’UNIVERSITENiceSophiaAntipolis
Discipline: (ouspe´cialite´)AsrophysiqueRelativiste
pre´sente´eetsoutenuepar
AUTEURAnastasiaFILINA
tudying explosive phenomena in astrophysics by the
S
example of gamma ray bursts and supernovae
-
The`sedirige´eparPascalCHARDONNET
soutenuele01/07/2015
Jury:
ChardonnetPascal LAPTH,Annecy-le-Vieux,France Directeur
ChechetkinValery KIAM,Moscow,Russia Co-directeur
ChetverushkinBoris KIAM,Moscow,Russia Membredejury
DellaValleMassimo OACN-INAF,Naples,Italy Rapporteur
NarozhnyNikolay MEPhI,Moscow,Russia Membredejury
PozanenkoAlexei IKI,Moscow,Russia Membredejury
TitarchukLev GMU-SPACS,Virginia,USA Rapporteur
VakiliFarrokh OCA,Nice,France Membredejury
i
Contents
Contents ii
ListofFigures iv
ListofTables vii
Abstract viii
1 Introduction 1
1.1 Supernovaeandgamma-raybursts . . . . . . . . . . . . . . . . . . . . . . . . 1
1.1.1 Observations . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 3
1.1.2 Physicalprocesses . . . . . . . . . . . . . . . . . . . . . . . . . . . . 7
1.1.3 Nucleosynthesis . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 9
1.2 Thesisoutline . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 10
2 Explosivephenomenainstellarphysics 12
2.1 Differentmodesofcombustion . . . . . . . . . . . . . . . . . . . . . . . . . . 13
2.2 Theroleofinstabilities . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 24
2.2.1 Rayleigh-Taylorinstability . . . . . . . . . . . . . . . . . . . . . . . . 24
2.2.2 Landau-Darrieusinstability . . . . . . . . . . . . . . . . . . . . . . . 26
2.2.3 Thermal-pulsationalinstability . . . . . . . . . . . . . . . . . . . . . . 26
2.2.4 Pairinstability . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 27
3 Asphericalnucleosynthesisinacore-collapsesupernovawith25 M standardpro-
⊙
genitor 28
3.1 Introduction . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 28
3.2 Methods . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 29
3.2.1 PiecewiseParabolicMethodonaLocalstencilforhydrodynamics . . . 29
3.2.2 Conjugategradientsforself-gravity . . . . . . . . . . . . . . . . . . . 30
3.2.3 Tracerparticlesmethodfornucleosynthesis . . . . . . . . . . . . . . . 30
3.3 Explosivenucleosynthesis . . . . . . . . . . . . . . . . . . . . . . . . . . . . 31
3.3.1 Networkofnuclearreactions . . . . . . . . . . . . . . . . . . . . . . . 31
3.3.2 Nuclearabundances . . . . . . . . . . . . . . . . . . . . . . . . . . . 33
3.3.3 Solvingreactionnetworkfornucleosynthesis . . . . . . . . . . . . . . 34
3.4 SNmodel . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 36
3.5 Results. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 38
3.6 Conclusions . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 46
ii
Contents iii
4 Multidimensionalsimulationsofpair-instabilitysupernovae 49
4.1 Introduction . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 49
4.2 Pair-instabilitysupernovae . . . . . . . . . . . . . . . . . . . . . . . . . . . . 50
4.3 Numericalapproach . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 51
4.3.1 Modellingin1D . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 52
4.3.2 Numericalexplosioninmulti-D . . . . . . . . . . . . . . . . . . . . . 54
4.4 Discussionsandconclusions . . . . . . . . . . . . . . . . . . . . . . . . . . . 58
5 OnGRBSpectra 59
5.1 Introduction: snapshotofGRBspectrum . . . . . . . . . . . . . . . . . . . . . 59
5.2 Black-bodyandThermalBremsstrahlungemission . . . . . . . . . . . . . . . 61
5.2.1 OurModel . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 62
5.3 Analysisofgamma-raybursts . . . . . . . . . . . . . . . . . . . . . . . . . . 63
5.3.1 AnalysisofGRB090618 . . . . . . . . . . . . . . . . . . . . . . . . . 63
5.4 AnalysisofsomeotherGRBs. . . . . . . . . . . . . . . . . . . . . . . . . . . 64
5.5 Discussionsandconclusions . . . . . . . . . . . . . . . . . . . . . . . . . . . 67
6 CosmologywithGRBs 74
6.1 Generalintroductiontocosmology . . . . . . . . . . . . . . . . . . . . . . . . 74
6.2 CosmologywithGRBs . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 81
6.3 NumberofGRBsperredshift . . . . . . . . . . . . . . . . . . . . . . . . . . . 82
6.3.1 Luminosityfunction . . . . . . . . . . . . . . . . . . . . . . . . . . . 85
6.3.2 RateofGRB . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 86
6.4 Conclusions . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 87
7 Generalconclusions 89
AnalysisofsomeGRBs 91
Abbreviations 100
PhysicalConstants 101
Symbols 102
Bibliography 103
Acknowledgements 115
List of Figures
1.1 Supernovaspectraltypes. Credit:DanielKasen . . . . . . . . . . . . . . . . . 5
1.2 A mosaic of HST images of the hosts of forty-two bursts (left) and the super-
novaehosts(right)(Fruchteretal.2006) . . . . . . . . . . . . . . . . . . . . 6
1.3 Illustrationofthelightcurvesofavarietyofsupernovaeontheleft(Smithetal.
2007)andcomparisonitwithGRBsontheright(Bloometal.2009). . . . . . 7
1.4 SampleoflightcurvesofbrightBATSEbursts,showinghighdiversity. . . . . 9
2.1 Curvesofconstantshockwavevelocity,calledRayleighlines. . . . . . . . . . . 14
2.2 TheshockadiabaticortheHugoniotadiabaticandRayleighline(dashed).. . . 16
2.3 The detonation adiabatic (continuous line) and the ordinary shock adiabatic
(dashedline). . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 18
2.4 Therelationbetweenthedifferentmodesofcombustion . . . . . . . . . . . . . 22
2.5 Example of Rayleigh-Taylor instability simulations by the PPML code Popov
(2012). Thedensitymapisshown . . . . . . . . . . . . . . . . . . . . . . . . 25
2.6 Example of Landau-Darrieus instability simulations for the C/O flame (Bell et
al.2004). Inflowboundaryconditionsinjectfuelintothebottomofthedomain.
They-velocityofthematerialwithrespecttotheplanarflameisshownincolor
fordifferentmomentsoftime. . . . . . . . . . . . . . . . . . . . . . . . . . . 26
3.1 Asimplifiednetworkofnuclearreactionsfrom12C to56Ni. . . . . . . . . . . . 32
3.2 Comparisonofournucleosynthesiscomputingcode(onthetop)andnucleosyn-
thesis computing code from Timmes et al. (2000) (on the bottom). As an ex-
ample we take evolution of the mass fractions under adiabatic expansion. The
initial conditions are T = 3 109 K, ρ = 1 109 g cm 3 and an initially half
−
× ×
12C -half16Ocompositionforthe13isotopeα-chainnetwork. . . . . . . . . 35
3.3 Presupernovaconfiguration. . . . . . . . . . . . . . . . . . . . . . . . . . . . 36
3.4 Densitydistributionfort = 60.5safterinducingtheexplosion. Thecoordinates
areshownintheunitsofsolarradius. Colorrepresentsthelogarithmofdensity
intheunitsofρ = 4.5 105 g/cm3. . . . . . . . . . . . . . . . . . . . . . . . 39
c
×
3.5 Temperaturedistributionforthesamemomentandinthesamecoordinateunits
asonfig.3.4. Colorrepresentsthelogarithmoftemperatureintheunitsof109 K. 39
3.6 Tracer locations and the density map for t = 60.5 s, reconstructed from the
recordedtracersdata. Colorrepresentsthetemperatureintheunitsof109 K. . . 40
3.7 Distributionof56Niand52Femassfractionsinvelocitymapfort = 60.5s. . . 41
3.8 Distributionof48Crand44Timassfractionsinvelocitymapfort = 60.5s.. . . 42
3.9 Distributionof40Caand36Armassfractionsinvelocitymapfort = 60.5s. . . 42
3.10 Distributionof32S and28Simassfractionsinvelocitymapfort = 60.5s. . . . 43
3.11 Distributionof24Mgand20Nemassfractionsinvelocitymapfort = 60.5s. . . 43
3.12 Distributionof16Oand12C massfractionsinvelocitymapfort = 60.5s. . . . 44
iv
ListofFigures v
3.13 Distributionof4Hemassfraction fort = 60.5s. Thenumbersshow thevalues
insomeregions. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 44
3.14 Theschematicplotofmainregionsintheejectaafterexplosion . . . . . . . . . 45
3.15 Comparison between the yields in our SN model (red line) and in a SN model
ofMaedaetal. (2002)(blueline). Thetotalmassoftheproducednucleiinthe
unitsof M inlogarithmicscaleisshown. . . . . . . . . . . . . . . . . . . . . 47
⊙
4.1 Fate of a star depending on its mass, M , and binding energy, E . Explosion
c bind
ismarkedbydiamondsandcollapseismarkedbycircles. . . . . . . . . . . . . 54
4.2 Nuclearenergyreleaseasafunctionofmaximumtemperature(diamonds). The
slope E T2 is shown. For comparison data from Arnett (1996) (stars) and
∝
Oberetal.(1983)(triangles)areshown. . . . . . . . . . . . . . . . . . . . . . 55
4.3 SN model with central ignition for t = 28 sec. Logarithm of density (a) is
shown in units of ρ = 2.65 105 g/cm3. Temperature (b) is shown in units of
c
×
T = 2.36 109 K. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 56
c
×
4.4 SN model with multicore ignition for t = 28 sec. Logarithm of density (a) is
shown in units of ρ = 2.65 105 g/cm3. Temperature (b) is shown in units of
c
×
T = 2.36 109 K. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 57
c
×
5.1 Time-integratedspectraGRB090618 . . . . . . . . . . . . . . . . . . . . . . 64
5.2 Time-integrated spectra for the different time intervals: from 0 to 50 s, from
50 to 59 s, from 59 to 69 s after the trigger time of GRB 090618. Blue line
showsthefitwiththeBandfunction(Eq5.1),orangelineshowstheblackbody
+bremsstrahlung(Eq.5.9). . . . . . . . . . . . . . . . . . . . . . . . . . . . . 65
5.3 Time-integrated spectra for the different time intervals: from 69 to 78 s, from
79 to 105 s after the trigger time of GRB 090618. Blue line shows the fit
with the Band function (Eq 5.1), orange line shows the fit with blackbody +
bremsstrahlung(Eq.5.9). . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 66
5.4 ThetemperatureevolutionwithtimeT(t)ofGRB090618 . . . . . . . . . . . . 67
5.5 ExampleoflightcurveofGRB090618(Izzoetal.2012) . . . . . . . . . . . . 67
5.6 Hot spots randomly appear on the surface of exploding star. Each spot pro-
ducesspikeofemission. Signalsfromthesespotsarriveatdifferenttimes,soan
observerseesthesuperpositionofthespikes. . . . . . . . . . . . . . . . . . . 70
5.7 2Dsimulationofanexplosionofa100solarmasspairinstabilitysupernovaeex-
plosioninthemulticoreexplosionscenariousingPPMLmethods. Thispicture
showsthefragmentationofthecoreandhotspotregionsofveryhightempera-
ture. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 71
5.8 Cartoon representation of a possible emission mechanism with Black-Body +
Bremmstrahlungemission . . . . . . . . . . . . . . . . . . . . . . . . . . . . 72
6.1 Amatirelationwithredshiftdistribution . . . . . . . . . . . . . . . . . . . . . 82
6.2 IsotropicequivalentradiatedenergyfromredshiftE (z) . . . . . . . . . . . . 82
iso
6.3 Comparison of luminosity distance computed from Amati relation” and from
cosmologicalredshiftbyeq.6.42 . . . . . . . . . . . . . . . . . . . . . . . . . 83
6.4 ”Volumetricfactor” dV/dz(z) . . . . . . . . . . . . . . . . . . . . . . . . . . . 85
1+z
6.5 IntegralofLuminosityFunctionfrom Campisietal.(2010)and Wanderman&
Piran(2010) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 86
6.6 RateGRBfrom Hopkins&Beacom(2006)andratePISNfrom Hummeletal.
(2012) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 87
ListofFigures vi
6.7 NumberofobservedGRBswithredshiftin(z,z+dz)overaredshiftinterval . . 87
1 ThetemperatureevolutionwithtimeT(t)ofGRB101023 . . . . . . . . . . . . 91
2 LightcurveofGRB101023(Penacchionietal.2012) . . . . . . . . . . . . . . 91
3 Spectral analysis of GRB 101023 for different intervals of time: [0-45 s] and
[45-89 s]. Blue line shows the fit with the Band function (Penacchioni et al.
2012),orangelineshowsthefitwithblackbody+bremsstrahlung . . . . . . . 92
4 Time-integratedspectraofGRB970111forthetimeintervalfrom21to24saf-
terthetriggertime. BluelineshowsthefitwiththeBandfunction(Eq5.1)(Fron-
tera et al. 2012), orange line shows the fit with blackbody + bremsstrahlung
(Eq.5.9). . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 93
5 ThetemperatureevolutionwithtimeT(t)ofGRB970111 . . . . . . . . . . . . 93
6 LightcurveofGRB970111detectedwithBATSE(Fronteraetal.2012) . . . . 93
7 GRB 970111. Time-integrated spectra for different intervals of time: 4-7 s, 7-
13 s, 13-16 s, 16-21 s, 21-24 s, 24-28s, 28-32s, 32-45 s. Blue line shows the
fit with the Band function (Eq 5.1), orange line shows the fit with blackbody +
bremsstrahlung(Eq.5.9). . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 94
8 Time-integrated spectraof GRB090926A forthe time intervalfrom 9.8 to10.5
s after the trigger time. Blue line shows the fit with the Band function (Eq 5.1)
(Tierneyetal.2013),orangelineshowsthefitwithblackbody+bremsstrahlung
(Eq.5.9). . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 95
9 ThetemperatureevolutionwithtimeT(t)ofGRB090926A . . . . . . . . . . . 95
10 LightcurveofGRB090926A(Tierneyetal.2013) . . . . . . . . . . . . . . . 95
11 GRB090926A.Time-integratedspectrafordifferentintervalsoftime: form0.0
to 3.3 s, 3.3 to 9.8 s, 9.8 to 10.5 s and 10.5 to 21.6 s. Blue line shows the fit
with the Band function (Eq 5.1), orange line shows the fit with blackbody +
bremsstrahlung(Eq.5.9). . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 96
12 ThetemperatureevolutionwithtimeT(t)ofGRB990510 . . . . . . . . . . . . 96
13 LightcurveofGRB990510(Fronteraetal.2012) . . . . . . . . . . . . . . . . 96
14 Time-integrated spectra of GRB990510 for the time intervals. Blue line shows
thefitwiththeBandfunction(Eq5.1),orangelineshowsthefitwithblackbody
+bremsstrahlung(Eq.5.9). . . . . . . . . . . . . . . . . . . . . . . . . . . . . 97
15 ThetemperatureevolutionwithtimeT(t)ofGRB980329 . . . . . . . . . . . . 98
16 LightcurveofGRB980329(Fronteraetal.2012) . . . . . . . . . . . . . . . . 98
17 Time-integrated spectra of GRB980329 for the time intervals. Blue line shows
thefitwiththeBandfunction(Eq5.1),orangelineshowsthefitwithblackbody
+bremsstrahlung(Eq.5.9). . . . . . . . . . . . . . . . . . . . . . . . . . . . . 99
List of Tables
3.1 Detailednucleosynthesisyields. . . . . . . . . . . . . . . . . . . . . . . . . . 46
4.1 Presupernovamodelsandparametersofexplosion . . . . . . . . . . . . . . . . 53
5.1 SpectralanalysisofGRB090618 . . . . . . . . . . . . . . . . . . . . . . . . . 68
vii
UNIVERSITENICE-SOPHIAANTIPOLIS-UFRSciences
Abstract
EcoleDoctoraleenSciencesFondamentalesetAppliquees
DoctorofRelativisticAstrophysics
Studyingexplosivephenomenainastrophysicsbytheexampleofgamma-rayburstsand
supernovae
byAnastasiaFilina
The formation of the first stars hundreds of millions of years after the Big-Bang marks the end
of the so-called Dark Ages. Currently, we have no direct observations on how the primordial
stars (Population III stars) formed, but according to modern theory of stellar evolution these
stars should be very massive (about 100 M ). Population III stars also have a potential to
⊙
produce probably most energetic flashes in the Universe – gamma-ray bursts (GRBs). GRBs
mayprovideoneofthemostpromisingmethodstoprobedirectlyfinalstageoflifeofprimordial
stars. Today’stelescopescannotlookfarenoughintothecosmicpasttoobservetheformationof
thefirststars,butthenewgenerationoftelescopeswilltesttheoreticalideasabouttheformation
ofthefirststars.
Thanks to many years of observations and number of successful space missions we have good
GRB’sdata–statisticsofoccurrence,spectrum,lightcurves. Buttherearestillalotofquestions
inthetheoryofGRBs. WeknowthatasignificantfractionofGRBs,thesocalledlong-duration
GRBs,arerelatedtothedeathofstarsandthattheyareconnectedwithsupernovae. Sogamma-
rayburstsareoneoftheclassesofexplosiveprocessesinstellarphysicsthatshouldhavealotof
commonwithsupernovaeexplosions. InthatcaseGRBsshouldfollowthesamephysicallaws
of explosion as supernovae. This work tries to approach the problem of GRBs as a problem of
stellarexplosion.
Necessary instruments of studying stellar explosion were developed as a part of doctoral re-
search: code for solving systems of nuclear reaction equations was incorporated into hydro-
dynamical code. These tools were applied for supernovae simulations in order to find possible
connectionwithGRBs. BasingonanalysisofsupernovaesimulationsspectralanalysisofGRBs
wasperformed.
Chapter 1
Introduction
Thecharacteristictimescalesofthelifeofstars,frommillionstobillionsyears,don’tallowus
to trace the entire life cycle of any concrete star. But huge number of observed stars gives us
an opportunity to observe them at different stages of their existence - from initial formation by
condensation of molecular clouds and up to their death, which for some stars is marked by the
brightestflashes-supernovaeexplosions. Supernovaeexplosionsareoneofthemostpowerful
events in the universe. The fact that the supernovae explosions occur with a certain regularity
and that regularities were found between different events suggests that this phenomenon is a
naturalterminationofstellarevolution.
Anotherexampleofpromptenergeticprocessintheuniversearegamma-raybursts,whichwere
discoveredfewdecadesafterintroductionoftheconceptofsupernovae. Apparentlythesepow-
erful flashes of gamma-ray emission are also associated with explosions of stars. However,
there are significant differences between gamma-ray bursts and usual supernovae. Most of the
radiation is emitted in gamma rays, and the total energy radiated may be one or two orders of
magnitudelargerthaninusualsupernovae. (Assumingthattheradiationisisotropic).
Thesephenomenaaretwoexamplesofexplosiveprocessesinastrophysics,whichplayasignif-
icantroleinthehistoryandevolutionoftheuniverse.
1.1 Supernovae and gamma-ray bursts
The transient appearance of a ”new star” (nova) in place of sky where none had been observed
previously,wasknownbyastronomersforalongtime. Butdramaticshiftinourunderstanding
thescaleofthesephenomenaoccurredinthebeginningoftheXX-thcentury. Itwasrealizedthat
someofthesestarsarelocatedinothergalaxies,thereforetheirluminosityshouldbefeworder
ofmagnitudeshigherthaninusualnovae. Intheearly1930sFritzZwicky,whocoinedtheterm
1