Palla, F., Salpeter, E. E., and Stahler, S. W. (1983). Primordial star form<strong>at</strong>ion - <strong>The</strong> role <strong>of</strong> molecular hydrogen. ApJ, 271:632–641. Papaloizou, J. C. B. and Lin, D. N. C. (1995). <strong>The</strong>ory Of Accretion Disks I: Angular Momentum Transport Processes. ARA&A, 33:505–540. Pawlik, A. H., Milosavljević, M., and Bromm, V. (<strong>2011</strong>). <strong>The</strong> First Galaxies: Assembly <strong>of</strong> Disks and Prospects for Direct Detection. ApJ, 731:54–+. Penston, M. V. (1969). Dynamics <strong>of</strong> self-gravit<strong>at</strong>ing gaseous spheres-III. An- alytical results in the free-fall <strong>of</strong> isothermal cases. MNRAS, 144:425–+. Penzias, A. A. and Wilson, R. W. (1965). A Measurement <strong>of</strong> Excess Antenna Temper<strong>at</strong>ure <strong>at</strong> 4080 Mc/s. ApJ, 142:419–421. Peters, T., Banerjee, R., Klessen, R. S., Mac Low, M.-M., Galván-Madrid, R., and Keto, E. R. (2010). H II Regions: Witnesses to Massive Star Form<strong>at</strong>ion. ApJ, 711:1017–1028. Petrovic, J., Langer, N., Yoon, S., and Heger, A. (2005). Which massive stars are gamma-ray burst progenitors? A&A, 435:247–259. Pringle, J. E. (1981). Accretion discs in astrophysics. ARA&A, 19:137–162. Rees, M. J. (2006). Origin <strong>of</strong> cosmic magnetic fields. AN, 327:395–+. Rees, M. J. and Ostriker, J. P. (1977). Cooling, dynamics and fragment<strong>at</strong>ion <strong>of</strong> massive gas clouds - Clues to the masses and radii <strong>of</strong> galaxies and clusters. MNRAS, 179:541–559. Ripamonti, E., Haardt, F., Ferrara, A., and Colpi, M. (2002). Radi<strong>at</strong>ion from the first forming stars. MNRAS, 334:401–418. 198
Rollinde, E., Vangioni, E., and Olive, K. (2005). Cosmological Cosmic Rays and the Observed 6 Li Pl<strong>at</strong>eau in Metal-poor Halo Stars. ApJ, 627:666–673. Rollinde, E., Vangioni, E., and Olive, K. A. (2006). Popul<strong>at</strong>ion III Gener<strong>at</strong>ed Cosmic Rays and the Production <strong>of</strong> 6 Li. ApJ, 651:658–666. Ruderman, M. A. (1974). Possible Consequences <strong>of</strong> Near<strong>by</strong> Supernova Explo- sions for Atmospheric Ozone and Terrestrial Life. Sci., 184:1079–1081. Saigo, K., M<strong>at</strong>sumoto, T., and Umemura, M. (2004). <strong>The</strong> Form<strong>at</strong>ion <strong>of</strong> Pop- ul<strong>at</strong>ion III Binaries. ApJ, 615:L65–L68. Salv<strong>at</strong>erra, R., Della Valle, M., Campana, S., Chincarini, G., Covino, S., D’Avanzo, P., Fernández-Soto, A., and Guidorzi, C. e. a. (2009). GRB090423 <strong>at</strong> a redshift <strong>of</strong> z˜8.1. N<strong>at</strong>ure, 461:1258–1260. Schaller, G., Schaerer, D., Meynet, G., and Maeder, A. (1992). New grids <strong>of</strong> stellar models from 0.8 to 120 solar masses <strong>at</strong> Z = 0.020 and Z = 0.001. A&AS, 96:269–331. Schleicher, D. R. G., Banerjee, R., Sur, S., Arshakian, T. G., Klessen, R. S., Beck, R., and Spaans, M. (2010). Small-scale dynamo action during the form<strong>at</strong>ion <strong>of</strong> the first stars and galaxies. I. <strong>The</strong> ideal MHD limit. A&A, 522:A115+. Schlickeiser, R. (2002). Cosmic Ray Astrophysics. Astronomy and Astro- physics Library; Physics and Astronomy Online Library, Berlin. Schneider, R., Ferrara, A., N<strong>at</strong>arajan, P., and Omukai, K. (2002). First Stars, Very Massive Black Holes, and Metals. ApJ, 571:30–39. 199
- 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: Navarro, J. F. and White, S. D. M.
- Page 215 and 216: Simon, M., Ghez, A. M., Leinert, C.
- Page 217 and 218: Tanvir, N. R., Fox, D. B., Levan, A
- Page 219 and 220: Rays, volume 576 of Lecture Notes i
- Page 221 and 222: Zatsepin, G. T. and Kuz’min, V. A