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paper_id string | title string | authors list | abstract string | latex list | bibtex list |
|---|---|---|---|---|---|
astro-ph0001001 | Statistics of Turbulence from Spectral-Line Data Cubes | [
{
"author": "Alex Lazarian"
}
] | Emission in spectral lines can provide unique information on interstellar turbulence. Doppler shifts due to supersonic motions contain information on turbulent velocity field which is otherwise difficult to measure. However, the problem of separation of velocity and density fluctuations is far from being trivial. Using atomic hydrogen (HI) as a test case, I review techniques applicable to emission line studies with the emphasis on those that can provide information on the underlying {\em power spectra} of velocity and density. I show that recently developed mathematical machinery is promising for the purpose. Its application to HI shows that in cold neutral hydrogen the velocity fluctuations dominate the small scale structures observed in spectral-line data cubes and this result is very important for the interpretation of observational data, including the identification of clouds. Velocity fluctuations are shown to dominate the formation of small scale structures that can be erroneously identified as diffuse clouds. One may argue that the HI data is consistent with the Goldreich-Shridhar picture of magnetohydrodynamic turbulence, but the cascade from the scales of several kpc that this interpretation involves does not fit well in the current paradigm of energy injection. The issue whether magnetic field does make the turbulence anisotropic is still open, but if this is the case, I show that studies of emission lines can provide a reliable way of determining magnetic field direction. I discuss various techniques for studying interstellar turbulence using emission lines, e.g. spectral correlation functions, genus statistics and principal component analysis. | [
{
"name": "procl.tex",
"string": "%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%\n%\t\t\tprocl.tex\t\t\t%\n%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%\n\n\\documentstyle[procl]{article}\n\n\\input{psfig.sty}\n\n% A useful Journal macro\n\\def\\Journal#1#2#3#4{(#1) {#2} {\\bf #3}, #4... | [
{
"name": "astro-ph0001001.extracted_bib",
"string": "\\begin{thebibliography}{99}\n\\bibitem{} Adler, D. S. \\& Roberts, W. W. Jr. \\Journal{1992}{\\ApJ}{384}{95}\n\\bibitem{} Armstrong, J.M., Rickett, B.J., \\& Spangler, S.R.\n\\Journal{1995}{\\ApJ}{443}{209}\n\\bibitem{} Brand, P. \\& Wouterloot, J.G.A. ... |
astro-ph0001002 | On the inverse Compton scattering model of radio pulsars | [
{
"author": "G. J. Qiao$^{1,2}$"
},
{
"author": "R. X. Xu$^{1,2}$"
},
{
"author": "J. F. Liu$^{1,2}$"
},
{
"author": "J. L. Han$^{1,3}$"
},
{
"author": "B. Zhang$^{1,2}$"
}
] | Some characteristics of the inverse Compton scattering (ICS) model are reviewed. At least the following properties of radio pulsars can be reproduced in the model: core or central emission beam, one or two hollow emission cones, different emission heights of these components, diverse pulse profiles at various frequencies, linear and circular polarization features of core and cones. | [
{
"name": "qHK.tex",
"string": "\\documentstyle[11pt,newpasp,twoside]{article}\n\\pagestyle{myheadings}\n\\markboth{{\\it Qiao et. al.}}{{\\it ICS model of Pulsars}}\n\\begin{document}\n\n\\title{On the inverse Compton scattering model of radio pulsars}\n\n\\author{G. J. Qiao$^{1,2}$,\n R. X. Xu$^{1,... | [
{
"name": "astro-ph0001002.extracted_bib",
"string": "\\begin{thebibliography}{}\n\n\\bibitem{} Beskin, V.S., Gurevich, A.V., Istomin, Y.N., 1988,\n Ap\\&SS, 146, 205\n\n\\bibitem{} Liu, J.F., Qiao, G.J., Xu, R.X., 1999,\n Chin. Phys. Lett., 16, 541\n\n\\bibitem{} Lyne A.G., Manchester R.N., 1988,\n ... |
astro-ph0001003 | Dark Halo and Disk Galaxy Scaling Laws in Hierarchical Universes | [
{
"author": "Julio F. Navarro\\altaffilmark{1}"
}
] | % We use cosmological N-body/gasdynamical simulations that include star formation and feedback to examine the proposal that scaling laws between the total luminosity, rotation speed, and angular momentum of disk galaxies reflect analogous correlations between the structural parameters of their surrounding dark matter halos. The numerical experiments follow the formation of galaxy-sized halos in two Cold Dark Matter dominated universes: the standard $\Omega=1$ CDM scenario and the currently popular $\Lambda$CDM model. We find that the slope and scatter of the I-band Tully-Fisher relation are well reproduced in the simulations, although not, as proposed in recent work, as a result of the cosmological equivalence between halo mass and circular velocity: large systematic variations in the fraction of baryons that collapse to form galaxies and in the ratio between halo and disk circular velocities are observed in our numerical experiments. The Tully-Fisher slope and scatter are recovered in this model as a direct result of the dynamical response of the halo to the assembly of the luminous component of the galaxy. We conclude that models that neglect the self-gravity of the disk and its influence on the detailed structure of the halo cannot be used to derive meaningful estimates of the scatter or slope of the Tully-Fisher relation. Our models fail, however, to match the zero-point of the Tully-Fisher relation, as well as that of the relation linking disk rotation speed and angular momentum. These failures can be traced, respectively, to the excessive central concentration of dark halos formed in the Cold Dark Matter cosmogonies we explore and to the formation of galaxy disks as the final outcome of a sequence of merger events. Disappointingly, our feedback formulation, calibrated to reproduce the empirical correlations linking star formation rate and gas surface density established by Kennicutt, has little influence on these conclusions. Agreement between model and observations appears to demand substantial revision to the Cold Dark Matter scenario or to the manner in which baryons are thought to assemble and evolve into galaxies in hierarchical universes. %Star %formation is significantly attenuated in early collapsing clumps, but %still most baryons collapse at high redshift into dense disks which %subsequently merge to form the final galaxy. %As a result, simulated %galaxies of given luminosity are too massive and too compact to be %consistent with typical spirals. A much stronger feedback %prescription, one that affects substantially the cooling, accretion, %and conversion of baryons into stars in systems with circular %%velocities as large as $\sim 200$-$300$ km s$^{-1}$, seems required in %order to bring models into closer agreement with observations. % % | [
{
"name": "tfemapj.tex",
"string": "\\documentstyle[emulateapj]{article}\n\\singlespace\n%\\tighten\n%\\eqsecnum\n%\n% Macros\n%\n%\\newcommand{\\etal}{{et Pl.} \\thinspace}\n\\newcommand{\\etal}{{et al.~}}\n\\newcommand{\\eg}{{e.g.,} \\thinspace}\n\\newcommand{\\ie}{{i.e.,} \\thinspace}\n\\newcommand{\\Ms... | [
{
"name": "astro-ph0001003.extracted_bib",
"string": "\\begin{thebibliography}{}\n\n\\bibitem[]{} Barnes, J., Efstathiou, G., 1987, \\apj, 319, 575\n%\n\\bibitem[]{} Cole, S.M., Arag\\'on-Salamanca, A., Frenk, C.S., Navarro, J.F., \\& Zepf,\nS.E.\\ 1994, \\mnras, 271, 781\n%\n\\bibitem[]{} Cole S., \\& Lace... |
astro-ph0001004 | Theory of the Interaction of Planetary Nebulae with the Interstellar Medium | [
{
"author": "Ruth Dgani"
}
] | "The theory of the interaction of planetary nebulae with the interstellar medium is important for th(...TRUNCATED) | [{"name":"dgani.tex","string":"\\documentstyle[11pt,newpasp,twoside]{article}\n\\markboth{ Ruth Dgan(...TRUNCATED) | [] |
astro-ph0001005 | [] | [] | [] | ||
astro-ph0001006 | On the Clustering of GRBs on the Sky | [
{
"author": "Shiv K. Sethi$^1$"
},
{
"author": "S. G. Bhargavi$^2$"
},
{
"author": "and Jochen Greiner$^3$"
}
] | "The two-point correlation of the 4th (current) BATSE catalog (2494 objects) is calculated. It is sh(...TRUNCATED) | [{"name":"GP46.tex","string":"\\documentstyle[epsfig]{aipproc}\n\n\\begin{document}\n\n\\title{On th(...TRUNCATED) | [{"name":"astro-ph0001006.extracted_bib","string":"\\bibitem{greiner}Greiner, J. , {\\tt http://www.(...TRUNCATED) |
astro-ph0001007 | Wide Field CCD Surface Photometry of the Giant Elliptical Galaxy NGC 4472 in the Virgo Cluster | [{"author":"Eunhyeuk Kim"},{"author":"$^1$ Myung Gyoon Lee"},{"author":"$^1$Department of Astronomy"(...TRUNCATED) | "We present deep wide field ($16'.4 \\times 16'.4$ ) Washington $CT_1$ CCD surface photometry of the(...TRUNCATED) | [{"name":"Kim_m49surf.tex","string":"% mnsample.tex\n%% Author: Eunhyeuk Kim, Myung Gyoon Lee and Do(...TRUNCATED) | [{"name":"astro-ph0001007.extracted_bib","string":"\\begin{thebibliography}{}\n\\bibitem[Barsony 198(...TRUNCATED) |
astro-ph0001008 | [] | "\\noindent{In 1997 the first optical afterglow of a cosmic Gamma-Ray Burst was discovered, and subs(...TRUNCATED) | [{"name":"astro-ph0001008.tex","string":"\\NeedsTeXFormat{LaTeX2e}\n\\documentclass[twoside]{article(...TRUNCATED) | [] | |
astro-ph0001009 | THE NATURE OF ULTRA-LUMINOUS COMPACT\\ X-RAY SOURCES IN NEARBY SPIRAL GALAXIES | [{"author":"Kazuo {\\sc Makishima}"},{"author":"Aya {\\sc Kubota}"},{"author":"Tsunefumi {\\sc Mizun(...TRUNCATED) | "Studies were made of {ASCA} spectra of seven ultra-luminous compact X-ray sources (ULXs) in nearby (...TRUNCATED) | [{"name":"ms.tex","string":"\\documentstyle[12pt,aasms4,psfig]{article}\n%\\documentstyle[12pt,aasms(...TRUNCATED) | [{"name":"astro-ph0001009.extracted_bib","string":"\\begin{thebibliography}{}\n\\setlength{\\itemsep(...TRUNCATED) |
astro-ph0001010 | Feedback Processes in the Early Universe | [{"author":"A. Ferrara\\inst{1}"},{"author":"B. Ciardi\\inst{2}"},{"author":"S. Marri\\inst{3}"},{"a(...TRUNCATED) | "Feedback effects due to massive stars and supernovae in the first objects are shown to strongly reg(...TRUNCATED) | [{"name":"esa99.tex","string":"%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%(...TRUNCATED) | [{"name":"astro-ph0001010.extracted_bib","string":"\\begin{thebibliography}{}\n\n\\bibitem[\\protect(...TRUNCATED) |
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