Hey! Thanks! This worked out perfectly!!!!
Now I have another question to you... The final file, which I got thanks to the help of all of you, is to be embedded into another web page... Which command should I add in the script to tell vi to embed it in the correct place? At the moment I do it by telling vi something like "go to line XXX, delete everything, insert text": :386,$d o <CTRL + v + ESC> :r /tmp/arXiV_2.txt :w! ~pau/WWW/arXiV.html But the inconvinient is that I have to modify the vim script whenever I add something to the web page, the number line 386 is wrong... and it is very tedious The place of the web page to embed it looks like this (without blank lines) : Between <!-- Fitxer viu comenca --> and <!-- Fitxer viu acaba --> --------------------------------------------------------------------------------------------------------------------------------- . . . . <font size=1.5 face=Verdana> <!-- Fitxer viu comenca --> <!-- comenca --> <br><a href="http://xxx.lanl.gov/pdf/astro-ph/0605080";> astro-ph/0605080</a> <br> <b>Títol/<i>Title</i>:</b> Populating the Galaxy with low-mass X-ray binaries <br> <b>Autors/<i>Authors</i>:</b> Paul D. Kiel, Jarrod R. Hurley <br> <b>Comentaris/<i>Comments</i>:</b> 17 pages and 9 figures; accepted by MNRAS <br> <br> We perform binary population synthesis calculations to investigate <br> the incidence of low-mass X-ray binaries and their birth rate in <br> the Galaxy. We use a binary evolution algorithm that models all <br> the relevant processes including tidal circularization and <br> synchronization. Parameters in the evolution algorithm that are <br> uncertain and may affect X-ray binary formation are allowed to <br> vary during the investigation. We agree with previous studies that <br> under standard assumptions of binary evolution the formation rate <br> and number of black-hole low-mass X-ray binaries predicted by the <br> model are more than an order of magnitude less than what is <br> indicated by observations. We find that the common-envelope <br> process cannot be manipulated to produce significant numbers of <br> black-hole low-mass X-ray binaries. However, by simply reducing <br> the mass-loss rate from helium stars adopted in the standard <br> model, to a rate that agrees with the latest data, we produce a <br> good match to the observations. Including low-mass X-ray binaries <br> that evolve from intermediate-mass systems also leads to <br> favourable results. We stress that constraints on the X-ray binary <br> population provided by observations are used here merely as a <br> guide as surveys suffer from incompleteness and much uncertainty <br> is involved in the interpretation of results. <br> <br> <br> <br><a href="http://xxx.lanl.gov/pdf/astro-ph/0605093";> astro-ph/0605093</a> <br> <b>Títol/<i>Title</i>:</b> Toroidal LNRF-velocity profiles in thick accretion discs <br> orbiting rapidly rotating Kerr black holes <br> <b>Autors/<i>Authors</i>:</b> Zdenek Stuchlik, Petr Slany, Gabriel Torok <br> <b>Comentaris/<i>Comments</i>:</b> Updated version of the Section talk at Albert Einstein <br> Century International Conference at Palais de l'Unesco, Paris, <br> France, 18-23 July, 2005; to appear in the Proceedings; AIP style <br> files included; 8 pages <br> <br> We show that in the equatorial plane of marginally stable thick <br> discs (with uniformly distributed specific angular momentum the <br> orbital velocity relative to the locally non-rotating frames <br> (LNRF) has a positive radial gradient in the vicinity of black <br> holes with spin a>0.99979. The change of sign of the velocity <br> gradient occurs just above the center of the thick toroidal discs, <br> in the region where stable circular geodesics of the Kerr <br> spacetime are allowed. The global character of the phenomenon is <br> given in terms of topology changes of the von Zeipel surfaces <br> (equivalent to the equivelocity surfaces in the tori with constant <br> specific angular momentum distribution). Toroidal von Zeipel <br> surfaces exist around the circle corresponding to the minimum of <br> the equatorial LNRF velocity profile, indicating a possibility of <br> development of some vertical instabilities in those parts of <br> marginally stable tori with positive gradient of the LNRF <br> velocity. Eventual oscillatory frequencies connected with the <br> phenomenon are given in a coordinate-independent form. <br> <br> <br> <br><a href="http://xxx.lanl.gov/pdf/astro-ph/0605094";> astro-ph/0605094</a> <br> <b>Títol/<i>Title</i>:</b> Basic properties of toroidal structures in Kerr--de Sitter <br> backgrounds <br> <b>Autors/<i>Authors</i>:</b> Zdenek Stuchlik, Petr Slany <br> <b>Comentaris/<i>Comments</i>:</b> Updated version of the Section talk at Albert Einstein <br> Century International Conference at Palais de l'Unesco, Paris, <br> France, 18-23 July, 2005; to appear in the Proceedings; AIP style <br> files included; 8 pages <br> <br> Perfect fluid tori with uniform distribution of the specific <br> angular momentum orbiting the Kerr-de Sitter black holes or naked <br> singularities are studied. Closed equipotential surfaces <br> corresponding to stationary toroidal discs are allowed only in the <br> spacetimes admitting stable circular geodesics. The last closed <br> surface crosses itself in the cusp(s) enabling outflow(s) of <br> matter from the torus due to the violation of hydrostatic <br> equilibrium. The repulsive cosmological constant, $\Lambda >0$, <br> implies the existence of the outer cusp (with a stabilizing effect <br> on the tori because of "excretion", i.e., outflow of matter from <br> the torus into the outer space) and the strong collimation of open <br> equipotential surfaces along the rotational axis. Both the effects <br> take place nearby the so-called static radius where the <br> gravitational attraction is just balanced by the cosmic repulsion. <br> The plus-family discs (which are always corotating in the <br> black-hole backgrounds but can be counterrotating, even with <br> negative energy of the fluid elements, in some naked singularity <br> backgrounds) are thicker and more extended than the minus-family <br> ones (which are always counterrotating in all backgrounds). If the <br> parameters of naked-singularity spacetimes are very close to the <br> parameters of extreme black-hole spacetimes, the family of <br> possible disc-like configurations includes members with two <br> isolated discs where the inner one is always a counterrotating <br> accretion disc. Mass estimates for tori with nonrelativistic <br> adiabatic equation of state give limits on their central <br> mass-density, for which the approximation of test fluid is <br> adequate. <br> <br> <br> <br><a href="http://xxx.lanl.gov/pdf/astro-ph/0605100";> astro-ph/0605100</a> <br> <b>Títol/<i>Title</i>:</b> The Massive Star Population in the Giant HII Region Tol89 <br> in NGC5398 <br> <b>Autors/<i>Authors</i>:</b> F. Sidoli, L. J. Smith, P. A. Crowther <br> <b>Comentaris/<i>Comments</i>:</b> 22 pages, 15 figures and 8 tables. Accepted by MNRAS on <br> 2006 April 28 <br> <br> We present new high spectral resolution VLT/UVES spectroscopy and <br> archival HST/STIS imaging and spectroscopy of the giant HII region <br> Tol89 in NGC5398. <br> From optical and UV HST images, we find that the star-forming <br> complex as a whole contains at least seven young compact massive <br> clusters. We resolve the two brightest optical knots, A and B, <br> into five individual young massive clusters along our slit, A1-4 <br> and B1 respectively. From Starburst99 (Leitherer et al.) UV <br> spectral modelling, and nebular H beta equivalent widths in the <br> optical, we derive ages that are consistent with the formation of <br> two separate burst events, of ~4+/-1 Myr and <3 Myr for knots A <br> (A1-4) and B (B1). An LMC metallicity is measured for both knots, <br> while nebular HeII 4686 is observed in knot B and perhaps in knot <br> A. We detect underlying broad wings on the strongest nebular <br> emission lines indicating velocities up to 600 km/s. We estimate <br> that there are ~95 early WN stars and ~35 early WC stars in <br> Tol89-A, using empirical template spectra of LMC WR stars from <br> Crowther and Hadfield. Remarkably, we also detect ~ three mid WNs <br> in the smallest (mass) cluster in Tol89-A, A4. From the strength <br> of nebular H beta, we obtain N(O) ~690 and 2800 for knots A and B. <br> We also employ a complementary approach using Starburst99 models, <br> in which the O star content is inferred from the stellar <br> continuum, and the WR population is obtained from spectral <br> synthesis of optical WR features using the grids from Smith et al. <br> We find reasonable agreement between the two methods for the O <br> star content and the N(WR)/N(O) ratio but find that the WR subtype <br> distribution is in error in the Starburst99 models, with far too <br> few WN stars being predicted. We attribute this failure to the <br> neglect of rotational mixing in evolutionary models. [abridged] <br> <br> <!-- acaba --> <!-- Fitxer viu acaba --> </div> </div> </body> </html> ---------------------------------------------------------------------------------------------------------------------------------
