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Bibliography Abbasi, R. U., Abu-Zayyad, T., Allen, M., Amman, J. F., Archbold, G., Belov, K., Belz, J. W., Ben Zvi, S. Y., Bergman, D. R., Blake, S. A., and et al. (2008). First Observation of the Greisen-Zatsepin-Kuzmin Suppres- sion. Phys. Rev. Letters, 100(10):101101–+. Abel, T., Anninos, P., Zhang, Y., and Norman, M. L. (1997). Modeling primordial gas in numerical cosmology. New. Astron., 2:181–207. Abel, T., Bryan, G. L., and Norman, M. L. (2002). The Formation of the First Star in the Universe. Sci., 295:93–98. Ahn, K. and Shapiro, P. R. (2007). Does radiative feedback by the first stars promote or prevent second generation star formation? MNRAS, 375:881– 908. Alvarez, M. A., Bromm, V., and Shapiro, P. R. (2006). The H II Region of the First Star. ApJ, 639:621–632. Asplund, M., Lambert, D. L., Nissen, P. E., Primas, F., and Smith, V. V. (2006). Lithium Isotopic Abundances in Metal-poor Halo Stars. ApJ, 644:229–259. Balbus, S. A. and Hawley, J. F. (1991). A powerful local shear instability in weakly magnetized disks. I - Linear analysis. II - Nonlinear evolution. ApJ, 376:214–233. 182
Barkana, R. and Loeb, A. (2001). In the beginning: the first sources of light and the reionization of the universe. Phys.Rep., 349:125–238. Barnes, J. and Efstathiou, G. (1987). Angular momentum from tidal torques. ApJ, 319:575–600. Bate, M. R., Bonnell, I. A., and Price, N. M. (1995). Modelling accretion in protobinary systems. MNRAS, 277:362–376. Bate, M. R. and Burkert, A. (1997). Resolution requirements for smoothed particle hydrodynamics calculations with self-gravity. MNRAS, 288:1060– 1072. Beers, T. C. and Christlieb, N. (2005). The Discovery and Analysis of Very Metal-Poor Stars in the Galaxy. ARA&A, 43:531–580. Belczynski, K., Bulik, T., Heger, A., and Fryer, C. (2007). The Lack of Gamma-Ray Bursts from Population III Binaries. ApJ, 664:986–999. Belczynski, K., Bulik, T., and Rudak, B. (2004). The First Stellar Binary Black Holes: The Strongest Gravitational Wave Burst Sources. ApJ, 608:L45–L48. Bell, A. R. (1978a). The acceleration of cosmic rays in shock fronts. I. MNRAS, 182:147–156. Bell, A. R. (1978b). The acceleration of cosmic rays in shock fronts. II. MN- RAS, 182:443–455. Bell, A. R. and Lucek, S. G. (2001). Cosmic ray acceleration to very high energy through the non-linear amplification by cosmic rays of the seed mag- netic field. MNRAS, 321:433–438. 183
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Copyright by Athena Ranice Stacy 20
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New Insights into Primordial Star F
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Acknowledgments I first want to giv
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angular momentum to rotate at nearl
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2.4.2.5 Thermodynamics of accretion
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Chapter 7. Outlook 177 Bibliography
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List of Figures 2.1 Density project
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1.1 Motivation Chapter 1 Introducti
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leaving behind a neutron star or bl
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describe studies that have attempte
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CRs may therefore provide a pathway
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expected that some of the gas withi
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our numerical methodology in Chapte
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scattering is the major source of o
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portance. The reaction rates for an
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The size of the refinement levels h
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the sink a temperature and pressure
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same time, such as the fragments in
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Figure 2.2: Physical state of the c
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2.4.2 Protostellar accretion 2.4.2.
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Despite some amount of rotational s
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Figure 2.6: Velocity field of the c
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Figure 2.7: Disk mass vs. time sinc
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Figure 2.8: Angular momentum struct
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sink tform [yr] Mfinal [M⊙] rinit
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sink (∼ 4 M⊙) that merged with
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actual final mass of the star is li
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the average temperature of all part
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disk accretion onto a primordial pr
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Figure 2.12: Impact of feedback on
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Figure 2.13: Comparison of specific
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the central core, eventually compri
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extending our simulation to later t
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that such a non-primordial origin t
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impose an upper mass limit to Pop I
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we use a ray-tracing scheme to foll
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3.2.3 Sink Particle Method When an
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convenient way to directly measure
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where the sum now extends from the
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Figure 3.1: Evolution of various pr
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ased on the prescription of Omukai
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ate found at late times in our ‘n
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Figure 3.2: Evolution of various di
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Figure 3.3: Evolution of disk mass
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Figure 3.4: Temperature versus numb
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disk mass is able to level off in d
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Figure 3.6: Projected density and t
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onto the disk. The numerical experi
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that the I-front expands as an hour
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Figure 3.8: Evolution of various H
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˙ M∗ = 3πΣν, (3.18) where ν
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the discrete nature of the gas part
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stars. We also note that, despite t
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current computational limits. If ra
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the deaths of massive stars (see Wo
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It is apparent that the angular mom
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h = 0.7. To accelerate structure fo
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acc = Lres 50 AU, where: Lres 0.5
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years, up to several dynamical time
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sp = GM∗ c2 , (4.1) s where cs is
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Figure 4.2: Left: Angular momentum
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through the disk, and the disk is e
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steadily grows for the rest of the
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Fig. 4.5 shows these timescales for
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sink B. Once on the MS, the sink A
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Figure 4.6: Evolution of stellar ro
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sink M∗(5000 yr) [M⊙] M∗(10 5
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present here, particularly if the s
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the stars grow to larger masses (se
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Here, Σ is the disk surface densit
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which has already detected GRBs at
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M⊙. They find that the specific a
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Page 149 and 150: Figure 5.1: Top panels: Effective v
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Page 153 and 154: Using cs ∝ T 1/2 results in ρ
Page 155 and 156: Figure 5.4: Evolution of gas proper
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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
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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
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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 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
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