With energy outputs >~10^51 erg in 0.1-1000 seconds, Gamma-ray Bursts (GRBs) are the most powerful events yet observed in the Universe. As such they are potential probes of the very early Universe, back to the era of re-ionisation and the first stars, but at the same time they have been observed to span a wide range in luminosity and redshift from the relatively local Universe (z~0.0085) out to z~6.29. GRBs divide into two classes based primarily on their duration as measured by T90 (the time taken to observe 90% of the total burst fluence). Long bursts (L-GRBs) have T90>~2 seconds, and shorts (S-GRBs) T90<~2 seconds. Though much has been learned regarding long duration GRBs since the first afterglow discovery in 1997 (including their likely association with massive core collapse supernovae), much remains unknown regarding short duration GRBs. In this work, after a brief historical introduction and review, we present analyses of the angular cross-correlation on the sky of short GRBs from the BATSE catalogue with galaxies in the local Universe sampled from the PSCz Redshift Survey and the Third Reference Catalogue of Bright Galaxies (RC3). In particular we show that 20%+/-8% (1 sigma) of all BATSE short duration bursts (localised to 10 degrees or better) show correlation with galaxy samples (morphological T-type<=4) within ~112 Mpc. Our statistics thus provide evidence that a substantial fraction of BATSE short GRBs show a tendency to be associated with large scale structure on the sky traced by a variety of galaxy types. Short GRBs are believed to be produced in the final merger of compact object (neutron star-neutron star or neutron star-black hole) binaries, though other possible progenitors are known to exist. The short initial spike of a giant flare from a Soft Gamma Repeater (SGR) such as the December 27th 2004 event from SGR1806-20 would have been detectable by BATSE as a short GRB if it occurred in a galaxy within ~30-50 Mpc (assuming a distance to SGR1806-20 of 15 kpc). Using the observed luminosities and rates of Galactic SGR giant flares, as well as theoretical predictions for the rate of binary mergers, we investigate the ability of plausible Luminosity Functions (LF), singly and in combination, to reproduce our observed correlations and a cosmological S-GRB population. We find the correlations are best explained by a separate population of lower luminosity S-GRBs, with properties consistent with them being due to giant flares from extra-galactic SGRs. Overall predicted number counts are a good fit to the observed BATSE number counts, and furthermore, the wider redshift distribution is consistent with the early Swift S-GRB redshift distribution. The three closest GRBs which have been observed to date were all long duration bursts, and we have therefore also searched for cross-correlation signals between the BATSE long GRBs and local galaxies. The three nearby bursts shared several similar properties such as being under-luminous, spectrally soft and of low variability. We have therefore also investigated a subset of L-GRBs with light curve properties similar to these known nearby bursts. The whole sample is found to exhibit a correlation level consistent with zero (1 sigma upper limit=10%, equivalent to 144 bursts) out to a radius of ~155 Mpc, but a spectrally soft, low observed fluence and low variability subset shows a correlation level of 28%+/-16% (=50+/-28 bursts) within 155 Mpc. These results are consistent with low-luminosity, low-variability bursts being a separate sub-class of L-GRBs which may be much more prevalent in the local Universe than their high-luminosity, cosmologically distant counterparts. To investigate this further, we once again examined plausible luminosity functions for single and dual high and low luminosity populations, based on observed intrinsic rates from the literature. The local population was once again found only to be produced to a sufficient level (while maintaining consistency with the observed overall number counts) by a separate low luminosity population with intrinsic rates several hundred times greater than their cosmological counterparts. Constraining the models via the Swift overall redshift distribution instead of threshold-adjusted BATSE number counts showed that the dual LF models were able to produce excellent fits to the entire redshift distribution while adequately reproducing a local population. Finally, suggestions are made as to the direction future work may follow in order to build on these initial investigations, as well as to how observations with future missions and detectors such as Fermi (formerly GLAST), Advanced LIGO and LOFAR may shed further light on nearby GRBs.

Esta dissertação apresenta uma breve revisão introdutória de alguns aspectos importantes de astrofísica nuclear e da fenomenologia do plasma de quarks e glúons a baixas temperaturas. Acredita-se que tal estado da matéria existe no núcleo de estrelas de nêutron e possivelmente de outros objetos compactos em astrofísica. Uma equação de estado para tal sistema é derivada incluindo as influências dos condensados de glúon e do campo magnético que também é uma característica importante das estrelas de nêutron. Finalmente, essa equação de estado é aplicada para o estudo de estrutura estelar de estrelas compactas e alguns resultados importantes são discutidos. / This dissertation presents a brief introductory overview of some key aspects of nuclear astrophysics and of the phenomenology of the quark gluon plasma at cold temperatures which is believed to exist inside the core of neutron stars and possible other compact astrophysical objects. An equation of state for this state of matter is derived incluing the influence of gluon condensates and the magnetic field which is also an important characteristic of neutron stars. And finally this equation of state is applied to the study of compact stellar structure and some important results are discussed.

Among the different types of massive stars in advanced evolutionary stages is the enigmatic WN8h type. There are only a few Wolf–Rayet (WR) stars with this spectral type in our Galaxy. It has long been suggested that WN8h-type stars are the products of binary evolution that may harbor neutron stars (NS). One of the most intriguing WN8h stars is the runaway WR 124 surrounded by its magnificent nebula M1-67. We test the presence of an accreting NS companion in WR 124 using ~100 ks long observations by the Chandra X-ray observatory. The hard X-ray emission from WR 124 with a luminosity of L X ~ 1031 erg s−1 is marginally detected. We use the non-local thermodynamic equilibrium stellar atmosphere code PoWR to estimate the WR wind opacity to the X-rays. The wind of a WN8-type star is effectively opaque for X-rays, hence the low X-ray luminosity of WR 124 does not rule out the presence of an embedded compact object. We suggest that, in general, high-opacity WR winds could prevent X-ray detections of embedded NS, and be an explanation for the apparent lack of WR+NS systems.

Compact Objects (Neutron Stars) form in the last moments of a star's life, during the violent events known as supernovae. As the star's core fusion falters, matter undergoes a dramatic gravitational compression resulting in internal densities rivaling subatomic particles. Ever since their discovery in the mid-twentieth century, these highly magnetized and rapidly rotating balls of condensed matter have provided a bountiful playground for astronomers seeking out exotic physics. Neutron Stars that emit electromagnetic radiation are seen by observers as Pulsars, named such for the pulse of intensity as the pulsar's radiation beam passes into our line of sight. These beams are comprised of two unique regions with differing phenomenology; core emission that arises close to the pulsar polar cap and centered within the radiation beam, and higher altitude conal emission that lies along the beam's periphery. While pulsars can and do emit over a wide frequency range, most known pulsars are seen as radio sources, at sensitivities where studies of the pulsar single-pulses allows us to probe the rich details of the plasma-filled pulsar magnetosphere. Even then, the radio emission often has a steep spectra, restricting the frequencies in which radio telescopes can study pulsars. We have utilized the unmatched sensitivity of Arecibo Observatory to conduct a multi-frequency single-pulse survey, between 327 MHz and the novel 4.5 GHz, of Arecibo's brightest high-frequency pulsars. The broad frequency range and single-pulse resolutions have allowed us to set accurate beam classifications for these nearly two dozen pulsars while extending constraints on important population trends to higher frequencies. Several of the pulsars in our survey exhibit deviant behavior, and are thus useful as followup case studies to further our understanding of pulsar radio emission. One of the most interesting cases involves pulsar B0823+26, where we find evidence for an age-dependent death-line separating core and conal dominated pulsars, suggesting that the plasma generating capabilities of a pulsar changes as they age. For the other three, they fall in the ``Partial Cone'' class; a type of pulsar that is characterized by strong delays in their emission. We find that all three of these pulsars show evidence of core emission.

While the process that converts implosion into explosion in core collapse supernovae is poorly understood, their observed asphericity provides new constraints on the physics of these events. Since pulsars are rotating and magnetized neutron stars, there is no doubt that rotation and magnetic fields are inherent to the exploding engine. We have shown that magnetic field amplification is an inevitable by-product of the differential rotation that accompanies core-collapse. We performed 1D core-collapse simulations of rotating iron cores with various rotational profiles and velocities. We found that differential rotation was a generic feature of rotating iron core collapse. As a result, the magnetorotational instability (MRI) generates magnetic fields of order 10¹⁵⁻¹⁷ G in a few tens of milliseconds where the negative shear is the strongest. Although magnetic fields of order 10¹⁵⁻¹⁷ G are very strong, they are not strong enough to modify the equation of state of degenerate electron gas near the proto-neutron star. The corresponding MHD luminosity available is ~10⁵² erg s⁻¹, which can modify the explosion dynamics if the power is sustained for a fraction of a second. When rotational effects are included, we found that there is a critical iron core rotation rate that gives the most rapidly rotating proto-neutron star, faster than which the rotational velocity of the proto-neutron star decreases due to centrifugal support. This non-monotonic behavior of post-collapse core rotation suggests that the progenitor of the most rapidly rotating proto-neutron star is not the most rapidly rotating iron core, but that those iron cores with nearly the critical initial rotation rate may produce the maximum proto-neutron star rotation, the strongest magnetic fields, and the most robust supernova explosions. Even small rotation may induce non-axisymmetric instabilities, which drive magneto-acoustic flux in to the mantle, transporting enegy out of the proto-neutron star to the region near the stalled shock. Further implications for rotation and magnetic fields, pulsars and magnetars, and jet formation mechanisms are discussed. / text

L'étude du champ électromagnétique autour des étoiles à neutrons est l'une des méthodes vitales pour comprendre la physique des pulsars. Alors que la plupart des publications utilisent l'hypothèse d'un champ électromagnétique dipolaire centré standard, des études récentes se sont concentrées sur l'inclusion de composantes de champ multipolaire plus élevées et ont présenté une image plus générale pour les pulsars dans lesquels le moment du dipôle magnétique est décalé du centre de l'étoile. Ce travail discute des conséquences d'un dipôle magnétique rotatif excentré dans le vide en montrant diverses caractéristiques des lignes de champ magnétique et de l'émission de pulsar. Une étude à large bande du spectre du rayonnement pulsar est également présentée par la création de cartes des différentes régions d'émission des pulsars distinguées sur la base de leur fréquence dans le but principal de rechercher l'évolution du profil d'impulsion avec la fréquence. La thèse présente tous les résultats ci-dessus accompagnés des discussions nécessaires pour comprendre les modèles théoriques utilisés et les détails des méthodes numériques appliquées. / Studying the electromagnetic field around neutron stars is one of the vital methods to understand the physics of the pulsars. While major literature uses assumption of a standard centred dipolar electromagnetic field, recent studies have focused on including higher multipolar field components and have presented a more generalized picture for pulsars in which the magnetic dipole moment is shifted off from the centre of the star. This work discusses the consequences of an off centred rotating magnetic dipole in vacuum by showing various characteristic features of magnetic field lines and pulsar emission. A broadband spectrum study of pulsar radiation is also laid out by creating maps of different emission regions of pulsars distinguished on the basis of their frequency with the main aim of looking for the evolution of the pulse profile with frequency. The thesis presents all the above results accompanied by the necessary discussions to understand the theoretical models used and the details of the numerical methods applied.

Esta dissertação apresenta uma breve revisão introdutória de alguns aspectos importantes de astrofísica nuclear e da fenomenologia do plasma de quarks e glúons a baixas temperaturas. Acredita-se que tal estado da matéria existe no núcleo de estrelas de nêutron e possivelmente de outros objetos compactos em astrofísica. Uma equação de estado para tal sistema é derivada incluindo as influências dos condensados de glúon e do campo magnético que também é uma característica importante das estrelas de nêutron. Finalmente, essa equação de estado é aplicada para o estudo de estrutura estelar de estrelas compactas e alguns resultados importantes são discutidos. / This dissertation presents a brief introductory overview of some key aspects of nuclear astrophysics and of the phenomenology of the quark gluon plasma at cold temperatures which is believed to exist inside the core of neutron stars and possible other compact astrophysical objects. An equation of state for this state of matter is derived incluing the influence of gluon condensates and the magnetic field which is also an important characteristic of neutron stars. And finally this equation of state is applied to the study of compact stellar structure and some important results are discussed.

Les étoiles à neutrons ont été largement étudiées depuis que Baade and Zwicky ont postulé leur existence en 1934. Ces études ont été et sont réalisées à l'interface de différents domaines de la physique tels que : l'astrophysique en rayons X, l'observation des pulsars, la relativité générale et plus dernièrement les ondes gravitationnelles, la physique du solide, ainsi que la physique nucléaire. Dans cette thèse nous nous concentrerons sur la description des étoiles à neutrons dans le cadre de la physique nucléaire et précisément de la croûte interne de l'étoile. Ces étoiles sont caractérisées par une masse importante de l'ordre d'une à deux masses solaires dans un rayon de 10 km. Quant à leur structure interne elle peut être décrite en trois strates : la croûte externe, la croûte interne et le cœur. La croûte externe correspond à un réseau cristallin de noyaux atomiques et un gaz d'électrons relativistes. Vient ensuite la croûte interne, définie lorsque les noyaux de la croûte externe sont si riches en neutrons qu'ils les libèrent dans le milieu pour former un gaz. Ici, nous ne parlons plus de noyaux mais d'agrégats car tous les nucléons qui les composent ne sont plus systématiquement liés. Cette structure complexe et sa composition est à l'origine de nombreuses propriétés caractéristiques des étoiles à neutrons.C'est ainsi que nous construirons notre étude en trois parties. Tout d'abord nous commencerons par traiter le gaz de neutrons entourant les agrégats. Le gaz de neutrons que nous considérons uniforme ici est superfluide et devrait donc présenter un mode de Goldstone. Cette description sera effectuée à l'aide de la QRPA. Puis nous en viendrons à la description des agrégats. Dans ces conditions on s'attend à observer des cristaux de sphères, des cylindres et des plaques de matière nucléaire, que nous décrirons grâce à l'approximation ETF. Puis nous terminerons par la description de l'interaction entre les agrégats et le gaz au niveau dynamique, et ce dans le cadre de la théorie hydrodynamique. Ces résultats seront appliqués à l'astrophysique et en particuliers aux glitches. / Neutron stars have been extensively studied since Baade and Zwicky have proposed their existence in 1934. Their description is at the interface of numerous domains of physics, e.g., X-ray astrophysics, pulsar signal observation, general relativity and nowadays gravitational waves, solid state physics, and also nuclear physics. In this thesis we will concentrate on the nuclear physics description, especially of the inner crust. These stars are charaterized by their large mass from one to two solar masses, in a radius of 10 km. Their inner structure can be divded in three major layers: the outer crust, the inner crust and the core. The outer crust consists of nuclei coexisting with an electron gas to ensure charge neutrality. If one goes deeper into the crust, the ratio of neutrons with respect to the total nucleon number increases. Eventually, the excess of neutrons in the nuclei gets so high that they drip out from the nuclei and create a dilute neutron gas. From now on, we will speak of nuclear clusters instead of nuclei. This phenomenon defines the limit between the outer crust and the inner crust. This complicated structure and composition is at the origin of many characteristic properties of neutron stars. Hence, we will construct our work in three major parts. First, we start to account for the neutron gas surrounding the clusters, which we treat as uniform. Here, the neutron gas is assumed to be superfluid, and one can expect a Goldstone mode. This description will be done in the framework of QRPA. Second, we will focus on the study of properties of the clusters contained in the inner crust. Under these conditions we expect to see cystal of spheres, rods and plates of bound nucleons, that we will describe with the help of the ETF approximation. Third, we will finish by treating the interaction between the clusters and the gas with hydrodynamics. The results will be applied to astrophysics and in particular to glitches.

京都大学 / 0048 / 新制・課程博士 / 博士(理学) / 甲第20915号 / 理博第4367号 / 新制||理||1627(附属図書館) / 京都大学大学院理学研究科物理学・宇宙物理学専攻 / (主査)准教授 菅沼 秀夫, 教授 田中 貴浩, 教授 川合 光 / 学位規則第4条第1項該当 / Doctor of Science / Kyoto University / DFAM

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