The XMM-Newton/Chandra monitoring campaign of the Galactic center region

We present the first results of our X-ray monitoring campaign on a 1.7 square degree region centered on Sgr A* using the satellites XMM-Newton and Chandra. The purpose of this campaign is to monitor the behavior (below 10 keV) of X-ray sources (both persistent and transient) which are too faint to be detected by monitoring instruments aboard other satellites currently in orbit (e.g., Rossi X-ray Timing Explorer; INTEGRAL). Our first monitoring observations (using the HRC-I aboard Chandra) were obtained on June 5, 2005. Most of the sources detected could be identified with foreground sources, such as X-ray active stars. In addition we detected two persistent X-ray binaries (1E 1743.1-2843; 1A 1742-294), two faint X-ray transients (GRS 1741.9-2853; XMM J174457-2850.3), as well as a possible new transient source at a luminosity of a few times 1034 erg s-1. We report on the X-ray results on these systems and on the non-detection of the transients in follow-up radio data using the Very Large Array. We discuss how our monitoring campaign can help to improve our understanding of the different types of X-ray transients (i.e., the very faint ones)

Millisecond Oscillations in X-Ray Binaries

The first millisecond X-ray variability phenomena from accreting compact objects have recently been discovered with the Rossi X-ray Timing Explorer. Three new phenomena are observed from low-mass X-ray binaries containing low-magnetic-field neutron stars: millisecond pulsations, burst oscillations and kiloHertz quasi-periodic oscillations. Models for these new phenomena involve the neutron star spin, and orbital motion closely around the neutron star and rely explicitly on our understanding of strong gravity and dense matter. I review the observations of these new neutron-star phenomena and possibly related ones in black-hole candidates, and describe the attempts to use them to perform measurements of fundamental physical interest in these systems.Comment: 40 pages, 17 figures, 4 tables - submitted to the Annual Review of Astronomy and Astrophysics; to appear September 200

Influência do resfriamento dinâmico na medição da tensão limite de escoamento

Non-Newtonian fluids may present several complex characteristics, such as viscoelasticity, plasticity and thixotropy. Understanding the behaviour of these materials is essential to facilitate its applicability, since many of them are present in daily life, such as gels, chocolate, and mayonnaise. The material studied on the present work was an waxy crude oil. The oil, present in reservoirs located in deep water, when subjected to low temperatures during production shutdowns, precipitates its paraffin, creating a structure which may be very resistant to flow. Thus, the formed material may represent a great difficulty to production restart. The design of pumps and compressors used in these systems depend on a rheological property called yield stress and therefore, it is essential to obtain reliable values of this rheological parameter. However, the complex behaviour, and the dependence of the crude oil characteristics on the shearing and temperature history make this a challenging task. Besides these, other factors may influence the measurement of yield stress, as the effect of wall slip and if the cooling is static or dynamic. This work shows the variation of yield stress for tests with dynamic cooling. The imposition of a stress during cooling caused the reduction in yield stress 0. Increasing the imposed stress, 0 decreased until it reached a minimum. Next, it was noticed an increase in yield stress with increasing imposed stress. The experiments carried out in this work were made in a commercial stress control rheometer. The effect of wall slip was tested by comparing smooth and rough geometries and it was verified signs of its presence, with the reduction of yield stress for smooth geometries. The equation of Weissenberg-Rabinowitsch, used for correction of the inhomogeneity of the shear stress along the radius geometry, seemed to be not necessary for the demonstrated results.Fluidos não newtonianos podem apresentar diversas características complexas, como a viscoelasticidade, plasticidade e tixotropia. Entender o comportamento de materiais tão complexos é fundamental para facilitar sua aplicabilidade, já que muitos estão presentes no cotidiano das pessoas, como géis, chocolate e maionese. O material estudado no presente trabalho foi um petróleo parafínico. O petróleo, presente em bacias localizadas em águas profundas, quando submetido a baixas temperaturas durante paradas de produção, precipita suas parafinas dando origem a uma estrutura que pode ser muito resistente ao escoamento. Dessa forma, o material formado pode representar uma grande dificuldade para o reinício da produção. O dimensionamento das bombas e compressores utilizados para retomada da produção depende de uma propriedade reológica denominada tensão limite de escoamento e, por isso, é fundamental obter valores confiáveis desse parâmetro reológico. No entanto, o comportamento complexo, e a dependência das características do petróleo com o histórico de cisalhamento e temperatura tornam a tarefa desafiadora. Outros fatores podem influenciar na medição da tensão limite de escoamento, como o efeito do escorregamento na parede do sensor da geometria e se o resfriamento é estático ou dinâmico. Este trabalho mostra a variação da tensão limite de escoamento para ensaios com resfriamento dinâmico. A imposição de tensão durante o resfriamento causou a redução da tensão limite de escoamento 0. Elevando-se a tensão imposta, 0 reduziu até atingir um valor mínimo. Em seguida, percebeu-se um aumento da tensão limite de escoamento com o aumento da tensão imposta. Os experimentos realizados neste trabalho foram feitos em um reômetro comercial do tipo tensão controlada (“stress controlled”). O efeito de escorregamento da amostra foi testado comparando geometrias com superfícies lisas e ranhuradas e foi possível verificar sinais de sua presença, com a redução da tensão limite de escoamento para geometrias lisas. A equação de Weissenberg-Rabinowitsch, utilizada para correção da não homogeneidade da tensão de cisalhamento ao longo do raio da geometria, mostrou-se não necessária para os resultados demonstrados

NICER Discovers Spectral Lines during Photospheric Radius Expansion Bursts from 4U 1820−30: Evidence for Burst-driven Winds

© 2019. The American Astronomical Society. All rights reserved. We report the discovery with the Neutron Star Interior Composition Explorer (NICER) of narrow emission and absorption lines during photospheric radius expansion (PRE) X-ray bursts from the ultracompact binary 4U 1820-30. NICER observed 4U 1820-30 in 2017 August during a low-flux, hard spectral state, accumulating about 60 ks of exposure. Five thermonuclear X-ray bursts were detected, of which four showed clear signs of PRE. We extracted spectra during the PRE phases and fit each to a model that includes a Comptonized component to describe the accretion-driven emission, and a blackbody for the burst thermal radiation. The temperature and spherical emitting radius of the fitted blackbody are used to assess the strength of PRE in each burst. The two strongest PRE bursts (burst pair 1) had blackbody temperatures of ≈0.6 keV and emitting radii of ≈100 km (at a distance of 8.4 kpc). The other two bursts (burst pair 2) had higher temperatures (≈0.67 keV) and smaller radii (≈75 km). All of the PRE bursts show evidence of narrow line emission near 1 keV. By coadding the PRE phase spectra of burst pairs 1 and, separately, 2, we find, in both coadded spectra, significant, narrow, spectral features near 1.0 (emission), 1.7, and 3.0 keV (both in absorption). Remarkably, all the fitted line centroids in the coadded spectrum of burst pair 1 appear systematically blueshifted by a factor of 1.046 ±0.006 compared to the centroids of pair 2, strongly indicative of a gravitational shift, a wind-induced blueshift, or more likely some combination of both effects. The observed shifts are consistent with this scenario in that the stronger PRE bursts in pair 1 reach larger photospheric radii, and thus have weaker gravitational redshifts, and they generate faster outflows, yielding higher blueshifts. We discuss possible elemental identifications for the observed features in the context of recent burst-driven wind models

A millisecond pulsar in an X-ray binary system.

Ordinary radio pulsars' are neutron stars with magnetic fields of similar to 10(12) gauss and spin periods in the range 0.1 to 3 seconds. In contrast, millisecond radio pulsars(2) have much weaker fields (similar to 10(9) gauss) and faster, millisecond spire rates. For both types of pulsar, the energy driving the radio pulsations is thought to be derived from the rotation of the neutron star. The star gradually 'spins down' as energy is radiated away. Millisecond radio pulsars are often located in binary systems(3). In a widely accepted theoretical model(4,5), they started as ordinary pulsars which lose most of their magnetic field and were 'spun up' to millisecond periods by the accretion of matter from a companion star in an X-ray binary system. Evidence(6-11) for this model has gradually mounted, but direct proof-in the form of the predicted coherent millisecond X-ray pulsations in the persistent flux of are X-ray binary has been lacking, despite many searches(12-15). Here we report the discovery(16) of such a pulsar, confirming theoretical expectations. The source will probably become a millisecond radio pulsar when the accretion turns off completely.</p

Observatory science with eXTP

High Energy Astrophysic

Observatory science with eXTP

In this White Paper we present the potential of the enhanced X-ray Timing and Polarimetry (eXTP) mission for studies related to Observatory Science targets. These include flaring stars, supernova remnants, accreting white dwarfs, low and high mass X-ray binaries, radio quiet and radio loud active galactic nuclei, tidal disruption events, and gamma-ray bursts. eXTP will be excellently suited to study one common aspect of these objects: their often transient nature. Developed by an international Consortium led by the Institute of High Energy Physics of the Chinese Academy of Science, the eXTP mission is expected to be launched in the mid 2020s