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Ekström, S., Meynet, G., Maeder, A., and Barblan, F. (2008b). Evolution towards the critical limit and the origin of Be stars. A&A, 478:467–485. Field, G. B. (1995). Is the Dynamo Theory of the Galactic Magnetic Field Wrong? In A. Ferrara, C. F. McKee, C. Heiles, & P. R. Shapiro, editor, The Physics of the Interstellar Medium and Intergalactic Medium, volume 80 of Astronomical Society of the Pacific Conference Series, pages 1–+. Frebel, A., Aoki, W., Christlieb, N., Ando, H., Asplund, M., Barklem, P. S., Beers, T. C., Eriksson, K., Fechner, C., Fujimoto, M. Y., Honda, S., Ka- jino, T., Minezaki, T., Nomoto, K., Norris, J. E., and Ryan, S. G. (2005). Nucleosynthetic signatures of the first stars. Nature, 434:871–873. Frebel, A. and Bromm, V. (2010). Dwarf archaeology: Probing the first en- richment events with low-luminosity galaxies. MNRAS, submitted (arXiv: 1010.1261). Frebel, A., Johnson, J. L., and Bromm, V. (2007). Probing the formation of the first low-mass stars with stellar archaeology. MNRAS, 380:L40–L44. Frebel, A., Johnson, J. L., and Bromm, V. (2009). The minimum stellar metallicity observable in the Galaxy. MNRAS, 392:L50–L54. Fryer, C. L., Woosley, S. E., and Hartmann, D. H. (1999). Formation Rates of Black Hole Accretion Disk Gamma-Ray Bursts. ApJ, 526:152–177. Galván-Madrid, R., Peters, T., Keto, E. R., Mac Low, M.-M., Banerjee, R., and Klessen, R. S. (2011). Time variability in simulated ultracompact and hypercompact H II regions. MNRAS, in press. 188
Gao, L., White, S. D. M., Jenkins, A., Frenk, C. S., and Springel, V. (2005). Early structure in ΛCDM. MNRAS, 363:379–392. Ginzburg, V. L. and Syrovatskii, S. I. (1969). The origin of cosmic rays. Gordon and Breach, New York. Glover, S. (2005). The Formation Of The First Stars In The Universe. Space Sci. Rev., 117:445–508. Glover, S. C. O. and Abel, T. (2008). Uncertainties in H2 and HD chemistry and cooling and their role in early structure formation. MNRAS, 388:1627– 1651. Gnedin, N. Y., Ferrara, A., and Zweibel, E. G. (2000). Generation of the Pri- mordial Magnetic Fields during Cosmological Reionization. ApJ, 539:505– 516. Goodman, A. A., Benson, P. J., Fuller, G. A., and Myers, P. C. (1993). Dense cores in dark clouds. VIII - Velocity gradients. ApJ, 406:528–547. Gou, L. J., Mészáros, P., Abel, T., and Zhang, B. (2004). Detectability of Long Gamma-Ray Burst Afterglows from Very High Redshifts. ApJ, 604:508–520. Greif, T., Springel, V., White, S., Glover, S., Clark, P., Smith, R., Klessen, R., and Bromm, V. (2011). Simulations on a Moving Mesh: The Clustered Formation of Population III Protostars. ApJ, 737:75–+. Greif, T. H. and Bromm, V. (2006). Two populations of metal-free stars in the early Universe. MNRAS, 373:128–138. 189
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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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are initialized at high z with smal
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M⊙, where Nneigh 32 is the typic
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Figure 5.1: Top panels: Effective v
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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
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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
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Page 197 and 198: Barkana, R. and Loeb, A. (2001). In
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Page 201: Daigne, F., Olive, K. A., Silk, J.,
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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