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Register a new userImprints of neutron stars in the interstellar medium
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E. M. Reynoso
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We have carried out an HI survey towards X-ray central compact objects (CCOs) inside supernova remnants (SNRs) which shows that many of them are placed within local HI minima. The nature of these minima is not clear, but the most likely explanation is that the CCOs have evacuated the neighboring gas. This survey also allowed us to detect a weak, diffuse radio nebula inside the SNR Vela Jr, probably created by the winds of its associated CCO.
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Inversion of interstellar gas or dust columns measured along the path to stars distributed in distance and direction allows reconstructing the distribution of interstellar matter (ISM) in 3D. A low resolution IS dust map based on the reddening of 23,000 stars illustrates the potential of future maps. It reveals the location of the main IS clouds within $sim$1kpc and, owing to biases towards weakly reddened targets, regions devoid of IS matter. It traces the Local Bubble and neighboring cavities, including a giant, $geq$1000 pc long cavity located beyond the so-called $beta$CMa tunnel, bordered by the main constituents of the Gould belt (GB), the rotating and expanding ring of clouds and young stars, inclined by $sim$ 20$^{circ}$ to the galactic plane. From comparison with diffuse X-ray background and absorption data it appears that the giant cavity is filled with warm, ionized and dust-poor gas in addition to million K gas. This set of structures must reflect the main events that occurred in the past. It has been suggested that the Cretaceus-Tertiary mass extinction may be due to a gamma-ray burst (GRB) in the massive globular cluster (GC) 47 Tuc during its close encounter with the Sun $sim$70 Myrs ago. Given the mass, speed and size of 47 Tuc, wherever it crossed the Galactic plane it must have produced at the crossing site significant dynamical effects on the disk stars and IS clouds, and triggered star formation. Interestingly, first-order estimates suggest that the GB dynamics and age could match the consequences of the cluster crossing. Additionally, the giant ionized, dust-free cavity could be related to an intense flux of hard radiation, and dust-gas decoupling after the burst could explain the high variability and pattern of the D/H ratio in the nearby gaseous ISM. Future Gaia data should confirm or dismiss this hypothesis.
We present an extensive analysis of the gas-phase abundances and depletion behaviors of neutron-capture elements in the interstellar medium (ISM). Column densities (or upper limits to the column densities) of Ga II, Ge II, As II, Kr I, Cd II, Sn II, and Pb II are determined for a sample of 69 sight lines with high- and/or medium-resolution archival spectra obtained with the Space Telescope Imaging Spectrograph onboard the Hubble Space Telescope. An additional 59 sight lines with column density measurements reported in the literature are included in our analysis. Parameters that characterize the depletion trends of the elements are derived according to the methodology developed by Jenkins (2009; arXiv:0905.3173). (In an appendix, we present similar depletion results for the light element B.) The depletion patterns exhibited by Ga and Ge comport with expectations based on the depletion results obtained for many other elements. Arsenic exhibits much less depletion than expected, and its abundance in low-depletion sight lines may even be supersolar. We confirm a previous finding by Jenkins (2009; arXiv:0905.3173) that the depletion of Kr increases as the overall depletion level increases from one sight line to another. Cadmium shows no such evidence of increasing depletion. We find a significant amount of scatter in the gas-phase abundances of Sn and Pb. For Sn, at least, the scatter may be evidence of real intrinsic abundance variations due to s-process enrichment combined with inefficient mixing in the ISM.
Turbulence is ubiquitous in the insterstellar medium and plays a major role in several processes such as the formation of dense structures and stars, the stability of molecular clouds, the amplification of magnetic fields, and the re-acceleration and diffusion of cosmic rays. Despite its importance, interstellar turbulence, alike turbulence in general, is far from being fully understood. In this review we present the basics of turbulence physics, focusing on the statistics of its structure and energy cascade. We explore the physics of compressible and incompressible turbulent flows, as well as magnetized cases. The most relevant observational techniques that provide quantitative insights of interstellar turbulence are also presented. We also discuss the main difficulties in developing a three-dimensional view of interstellar turbulence from these observations. Finally, we briefly present what could be the the main sources of turbulence in the interstellar medium.
Debris discs are typically revealed through excess emission at infrared wavelengths. Most discs exhibit excess at mid- and far-infrared wavelengths, analogous to the solar systems Asteroid and Edgeworth-Kuiper belts. Recently, stars with strong (1 per cent) excess at near-infrared wavelengths were identified through interferometric measurements. Using the HIgh Precision Polarimetric Instrument (HIPPI), we examined a sub-sample of these hot dust stars (and appropriate controls) at parts-per-million sensitivity in SDSS g (green) and r (red) filters for evidence of scattered light. No detection of strongly polarized emission from the hot dust stars is seen. We therefore rule out scattered light from a normal debris disk as the origin of this emission. A wavelength dependent contribution from multiple dust components for hot dust stars is inferred from the dispersion (difference in polarization angle in red and green) of southern stars. Contributions of 17 ppm (green) and 30 ppm (red) are calculated, with strict 3 sigma upper limits of 76 and 68 ppm, respectively. This suggests weak hot dust excesses consistent with thermal emission, although we cannot rule out contrived scenarios, e.g. dust in a spherical shell or face on discs. We also report on the nature of the local interstellar medium, obtained as a byproduct of the control measurements. Highlights include the first measurements of the polarimetric colour of the local interstellar medium and discovery of a southern sky region with a polarization per distance thrice the previous maximum. The data suggest the wavelength of maximum polarization is bluer than typical.
Planetary Nebulae (PNe) are the result of heavy mass loss of the asymptotic giant branch (AGB) stars. They are understood in terms of Kwoks (1978) interacting-winds model as the product of the mass-loss history on the AGB and the central star (CS) evolution. Since the CS are close to the end of nuclear burning and at their hottest stage of evolution then, precise modeling of these pre-white dwarfs is a prerequisite in order to calculate reliable ionizing fluxes which are crucial input for the presently available 3D photoionization codes. In the framework of a systematic study of PNe which show evidence for an interaction with the ISM, we present a NLTE analysis of their CS.
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