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List of Tables 2.1 Formation times, final masses, and locations of the sinks. . . . 35 3.1 Formation times, final masses, and locations of sinks in ‘nofeedback’ case. . . . . . . . . . . . . . . . . . . . . . . . . . . . 80 3.2 Same as Table 3.1, but for sinks remaining at the end of the ‘with-feedback’ case. . . . . . . . . . . . . . . . . . . . . . . . 80 4.1 Final sink angular momenta, stellar masses, and stellar rotational velocities. . . . . . . . . . . . . . . . . . . . . . . . . . . 119 xii
List of Figures 2.1 Density projection of gas on various scales. . . . . . . . . . . . 20 2.2 Physical state of the collapsing core just prior to sink formation. 23 2.3 Radial structure of gas just prior to sink formation. . . . . . . 24 2.4 Kinematics of gas around the main sink particle. . . . . . . . . 26 2.5 Density and temperature projections of the star-forming disk. 28 2.6 Velocity field of the central gas distribution. . . . . . . . . . . 29 2.7 Disk mass versus time. . . . . . . . . . . . . . . . . . . . . . . 31 2.8 Angular momentum structure of star-forming gas. . . . . . . . 33 2.9 Sink mass and accretion rate versus time. . . . . . . . . . . . . 38 2.10 Evolution of gas thermodynamic properties. . . . . . . . . . . 40 2.11 Dominant cooling processes in the center of the minihalo. . . . 42 2.12 Impact of feedback on the accretion process. . . . . . . . . . . 45 2.13 Specific angular momentum profiles of gas for various cosmological simulations. . . . . . . . . . . . . . . . . . . . . . . . . 47 3.1 Evolution of various properties of the growing protostar according to our analytical model. . . . . . . . . . . . . . . . . . . . 65 3.2 Evolution of various disk properties. . . . . . . . . . . . . . . . 71 3.3 Evolution of disk mass over time. . . . . . . . . . . . . . . . . 73 3.4 Temperature versus number density for both cases at various times in the simulations. . . . . . . . . . . . . . . . . . . . . . 75 3.5 Projected density and temperature structure of central 10,000 AU without protostellar feedback. . . . . . . . . . . . . . . . . 78 3.6 Projected density and temperature structure of gas under LW and ionization feedback. . . . . . . . . . . . . . . . . . . . . . 79 3.7 Projected ionization structure of gas at 1700, 2300, and 4200 yr after initial sink formation. . . . . . . . . . . . . . . . . . . . 82 3.8 Evolution of various H ii region properties over time. . . . . . 85 3.9 Effect of radiative feedback on protostellar accretion. . . . . . 88 xiii
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: Chapter 7. Outlook 177 Bibliography
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
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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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Figure 5.2: Effect of relative stre
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Using cs ∝ T 1/2 results in ρ
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Figure 5.4: Evolution of gas proper
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a much smaller contribution from <
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abundances of HD, which also acts a
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first stars had very short lifetime
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of star-forming material. Here we t
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star formation, they found CR energ
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The GZK cutoff applies only to thos
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and virialization redshift zvir = 2
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and undergoes free-fall collapse. I
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β = 1 − −2 1/2 ɛ + 1 mHc2
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and where ΓCR(D) = 5 × 10 −29 e
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Figure 6.2: Thermal evolution of pr
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Figure 6.3: Minimum temperature rea
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Figure 6.4: Thermal evolution of pr
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The CR energy density can now be es
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2007). When considering realistic c
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6.3.5 Fragmentation scale As is evi
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2006). This decrease in fragmentati
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Chapter 7 Outlook Our understanding
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that Pop III stars likely experienc
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to be part of an area of scientific
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Barkana, R. and Loeb, A. (2001). In
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Bromm, V., Kudritzki, R. P., and Lo
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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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