Springel, V., Yoshida, N., and White, S. D. M. (2001). GADGET: a code for collisionless and gasdynamical cosmological simul<strong>at</strong>ions. New Astron., 6:79–117. Spruit, H. C. (2002). Dynamo action <strong>by</strong> differential rot<strong>at</strong>ion in a stably str<strong>at</strong>- ified stellar interior. A&A, 381:923–932. <strong>Stacy</strong>, A., Bromm, V., and Loeb, A. (<strong>2011</strong>). Rot<strong>at</strong>ion speed <strong>of</strong> the first stars. MNRAS, 413:543–553. <strong>Stacy</strong>, A., Greif, T. H., and Bromm, V. (2010). <strong>The</strong> first stars: form<strong>at</strong>ion <strong>of</strong> binaries and small multiple systems. MNRAS, 403:45–60. Stahler, S. W., Palla, F., and Salpeter, E. E. (1986). Primordial stellar evolu- tion - <strong>The</strong> protostar phase. ApJ, 302:590–605. Suda, T., Aikawa, M., Machida, M. N., Fujimoto, M. Y., and Iben, I. J. (2004). Is HE 0107-5240 A Primordial Star? <strong>The</strong> Characteristics <strong>of</strong> Ex- tremely Metal-Poor Carbon-Rich Stars. ApJ, 611:476–493. Suwa, Y. and Ioka, K. (2010). Can Gamma-Ray Burst Jets Break Out the First Stars? arXiv:1009.6001. Tan, J. C. and Blackman, E. G. (2004). Protostellar Disk Dynamos and Hydromagnetic Outflows in Primordial Star Form<strong>at</strong>ion. ApJ, 603:401–413. Tan, J. C. and McKee, C. F. (2004). <strong>The</strong> Form<strong>at</strong>ion <strong>of</strong> the First Stars. I. Mass Infall R<strong>at</strong>es, Accretion Disk Structure, and Protostellar Evolution. ApJ, 603:383–400. 202
Tanvir, N. R., Fox, D. B., Levan, A. J., Berger, E., Wiersema, K., Fynbo, J. P. U., Cucchiara, A., Krühler, T., Gehrels, N., Bloom, J. S., and Greiner, J. e. a. (2009). A γ-ray burst <strong>at</strong> a redshift <strong>of</strong> z˜8.2. N<strong>at</strong>ure, 461:1254–1257. Tegmark, M., Silk, J., Rees, M. J., Blanchard, A., Abel, T., and Palla, F. (1997). How Small Were the First Cosmological Objects? ApJ, 474:1–+. Tormen, G., Bouchet, F. R., and White, S. D. M. (1997). <strong>The</strong> structure and dynamical evolution <strong>of</strong> dark m<strong>at</strong>ter haloes. MNRAS, 286:865–884. Torn<strong>at</strong>ore, L., Ferrara, A., and Schneider, R. (2007). Popul<strong>at</strong>ion III stars: hidden or disappeared? MNRAS, 382:945–950. Torres, D. F., Boldt, E., Hamilton, T., and Loewenstein, M. (2002). Near<strong>by</strong> quasar remnants and ultrahigh-energy cosmic rays. Phys. Rev. D, 66(2):023001–+. Trac, H. and Gnedin, N. Y. (2009). Computer Simul<strong>at</strong>ions <strong>of</strong> Cosmic Reion- iz<strong>at</strong>ion. (arXiv: 0906.4348). Trenti, M. and Stiavelli, M. (2009). Form<strong>at</strong>ion R<strong>at</strong>es <strong>of</strong> Popul<strong>at</strong>ion III Stars and Chemical Enrichment <strong>of</strong> Halos during the Reioniz<strong>at</strong>ion Era. ApJ, 694:879–892. Tseliakhovich, D., Barkana, R., and Hir<strong>at</strong>a, C. (2010). Suppression and Sp<strong>at</strong>ial Vari<strong>at</strong>ion <strong>of</strong> Early Galaxies and Minihalos. (arXiv: 1012.2574). Tseliakhovich, D. and Hir<strong>at</strong>a, C. (2010). Rel<strong>at</strong>ive velocity <strong>of</strong> dark m<strong>at</strong>ter and baryonic fluids and the form<strong>at</strong>ion <strong>of</strong> the first structures. Phys. Rev. D, 82(8):083520–+. 203
- Page 1 and 2:
Copyright by Athena Ranice Stacy 20
- Page 3 and 4:
New Insights into Primordial Star F
- Page 5 and 6:
Acknowledgments I first want to giv
- Page 7 and 8:
angular momentum to rotate at nearl
- Page 9 and 10:
2.4.2.5 Thermodynamics of accretion
- Page 11 and 12:
Chapter 7. Outlook 177 Bibliography
- Page 13 and 14:
List of Figures 2.1 Density project
- Page 15 and 16:
1.1 Motivation Chapter 1 Introducti
- Page 17 and 18:
leaving behind a neutron star or bl
- Page 19 and 20:
describe studies that have attempte
- Page 21 and 22:
CRs may therefore provide a pathway
- Page 23 and 24:
expected that some of the gas withi
- Page 25 and 26:
our numerical methodology in Chapte
- Page 27 and 28:
scattering is the major source of o
- Page 29 and 30:
portance. The reaction rates for an
- Page 31 and 32:
The size of the refinement levels h
- Page 33 and 34:
the sink a temperature and pressure
- Page 35 and 36:
same time, such as the fragments in
- Page 37 and 38:
Figure 2.2: Physical state of the c
- Page 39 and 40:
2.4.2 Protostellar accretion 2.4.2.
- Page 41 and 42:
Despite some amount of rotational s
- Page 43 and 44:
Figure 2.6: Velocity field of the c
- Page 45 and 46:
Figure 2.7: Disk mass vs. time sinc
- Page 47 and 48:
Figure 2.8: Angular momentum struct
- Page 49 and 50:
sink tform [yr] Mfinal [M⊙] rinit
- Page 51 and 52:
sink (∼ 4 M⊙) that merged with
- Page 53 and 54:
actual final mass of the star is li
- Page 55 and 56:
the average temperature of all part
- Page 57 and 58:
disk accretion onto a primordial pr
- Page 59 and 60:
Figure 2.12: Impact of feedback on
- Page 61 and 62:
Figure 2.13: Comparison of specific
- Page 63 and 64:
the central core, eventually compri
- Page 65 and 66:
extending our simulation to later t
- Page 67 and 68:
that such a non-primordial origin t
- Page 69 and 70:
impose an upper mass limit to Pop I
- Page 71 and 72:
we use a ray-tracing scheme to foll
- Page 73 and 74:
3.2.3 Sink Particle Method When an
- Page 75 and 76:
convenient way to directly measure
- Page 77 and 78:
where the sum now extends from the
- Page 79 and 80:
Figure 3.1: Evolution of various pr
- Page 81 and 82:
ased on the prescription of Omukai
- Page 83 and 84:
ate found at late times in our ‘n
- Page 85 and 86:
Figure 3.2: Evolution of various di
- Page 87 and 88:
Figure 3.3: Evolution of disk mass
- Page 89 and 90:
Figure 3.4: Temperature versus numb
- Page 91 and 92:
disk mass is able to level off in d
- Page 93 and 94:
Figure 3.6: Projected density and t
- Page 95 and 96:
onto the disk. The numerical experi
- Page 97 and 98:
that the I-front expands as an hour
- Page 99 and 100:
Figure 3.8: Evolution of various H
- Page 101 and 102:
˙ M∗ = 3πΣν, (3.18) where ν
- Page 103 and 104:
the discrete nature of the gas part
- Page 105 and 106:
stars. We also note that, despite t
- Page 107 and 108:
current computational limits. If ra
- Page 109 and 110:
the deaths of massive stars (see Wo
- Page 111 and 112:
It is apparent that the angular mom
- Page 113 and 114:
h = 0.7. To accelerate structure fo
- Page 115 and 116:
acc = Lres 50 AU, where: Lres 0.5
- Page 117 and 118:
years, up to several dynamical time
- Page 119 and 120:
sp = GM∗ c2 , (4.1) s where cs is
- Page 121 and 122:
Figure 4.2: Left: Angular momentum
- Page 123 and 124:
through the disk, and the disk is e
- Page 125 and 126:
steadily grows for the rest of the
- Page 127 and 128:
Fig. 4.5 shows these timescales for
- Page 129 and 130:
sink B. Once on the MS, the sink A
- Page 131 and 132:
Figure 4.6: Evolution of stellar ro
- Page 133 and 134:
sink M∗(5000 yr) [M⊙] M∗(10 5
- Page 135 and 136:
present here, particularly if the s
- Page 137 and 138:
the stars grow to larger masses (se
- Page 139 and 140:
Here, Σ is the disk surface densit
- Page 141 and 142:
which has already detected GRBs at
- Page 143 and 144:
M⊙. They find that the specific a
- Page 145 and 146:
are initialized at high z with smal
- Page 147 and 148:
M⊙, where Nneigh 32 is the typic
- Page 149 and 150:
Figure 5.1: Top panels: Effective v
- Page 151 and 152:
Figure 5.2: Effect of relative stre
- Page 153 and 154:
Using cs ∝ T 1/2 results in ρ
- Page 155 and 156:
Figure 5.4: Evolution of gas proper
- Page 157 and 158:
a much smaller contribution from <
- Page 159 and 160:
abundances of HD, which also acts a
- Page 161 and 162:
first stars had very short lifetime
- Page 163 and 164:
of star-forming material. Here we t
- Page 165 and 166: star formation, they found CR energ
- Page 167 and 168: The GZK cutoff applies only to thos
- Page 169 and 170: and virialization redshift zvir = 2
- Page 171 and 172: and undergoes free-fall collapse. I
- Page 173 and 174: β = 1 − −2 1/2 ɛ + 1 mHc2
- Page 175 and 176: and where ΓCR(D) = 5 × 10 −29 e
- Page 177 and 178: Figure 6.2: Thermal evolution of pr
- Page 179 and 180: Figure 6.3: Minimum temperature rea
- Page 181 and 182: Figure 6.4: Thermal evolution of pr
- Page 183 and 184: The CR energy density can now be es
- Page 185 and 186: 2007). When considering realistic c
- Page 187 and 188: 6.3.5 Fragmentation scale As is evi
- Page 189 and 190: 2006). This decrease in fragmentati
- Page 191 and 192: Chapter 7 Outlook Our understanding
- Page 193 and 194: that Pop III stars likely experienc
- Page 195 and 196: to be part of an area of scientific
- Page 197 and 198: Barkana, R. and Loeb, A. (2001). In
- Page 199 and 200: Bromm, V., Kudritzki, R. P., and Lo
- Page 201 and 202: Daigne, F., Olive, K. A., Silk, J.,
- Page 203 and 204: Gao, L., White, S. D. M., Jenkins,
- Page 205 and 206: Heger, A., Woosley, S. E., and Spru
- Page 207 and 208: Kratter, K. M. and Murray-Clay, R.
- Page 209 and 210: Machida, M. N., Omukai, K., Matsumo
- Page 211 and 212: Navarro, J. F. and White, S. D. M.
- Page 213 and 214: Rollinde, E., Vangioni, E., and Oli
- Page 215: Simon, M., Ghez, A. M., Leinert, C.
- Page 219 and 220: Rays, volume 576 of Lecture Notes i
- Page 221 and 222: Zatsepin, G. T. and Kuz’min, V. A