Simulations of the W50-SS433 system

AbstractSupernovae and astrophysical jets are two of the most energetic and intriguing objects in the universe. We examine an interesting scenario that involves the interaction of these two extreme phenomena, motivated by observations of the W50-SS433 system: a jet launched from the microquasar SS433 (an X-ray binary) located inside a supernova remnant, W50. These observations revealed a unique morphology of the remnant, attributed to the presence of the jet. We performed full 3D relativistic hydrodynamic simulations to better capture the interaction between the remnant and the jet and post-processed the data with a radiative transfer code to create emission maps.

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MODELING JET INTERACTIONS WITH THE AMBIENT MEDIUM

Acta Polytechnica ◽

10.14311/ap.2013.53.0683 ◽

2013 ◽

Vol 53 (A) ◽

pp. 683-686

Author(s):

J. H. Beall ◽

J. Guillory ◽

D. V. Rose ◽

Michael T. Wolff

Keyword(s):

Large Scale ◽

Ambient Medium ◽

Time Dependent ◽

Complex Structures ◽

Relativistic Hydrodynamic ◽

Astrophysical Jets ◽

Hydrodynamic Simulations ◽

Central Engine ◽

Interstellar Material ◽

Jet Interactions

Recent high-resolution (see, e.g., [13]) observations of astrophysical jets reveal complex structures apparently caused by ejecta from the central engine as the ejecta interact with the surrounding interstellar material. These observations include time-lapsed “movies” of both AGN and microquasars jets which also show that the jet phenomena are highly time-dependent. Such observations can be used to inform models of the jet–ambient-medium interactions. Based on an analysis of these data, we posit that a significant part of the observed phenomena come from the interaction of the ejecta with prior ejecta as well as interstellar material. In this view, astrophysical jets interact with the ambient medium through which they propagate, entraining and accelerating it. We show some elements of the modeling of these jets in this paper, including energy loss and heating via plasma processes, and large scale hydrodynamic and relativistic hydrodynamic simulations.

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Can jets make the radioactively powered emission from neutron star mergers bluer?

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa3337 ◽

2020 ◽

Vol 500 (2) ◽

pp. 1772-1783

Author(s):

L Nativi ◽

M Bulla ◽

S Rosswog ◽

C Lundman ◽

G Kowal ◽

...

Keyword(s):

Monte Carlo ◽

Neutron Star ◽

Radiative Transfer ◽

Initial Conditions ◽

Heavy Elements ◽

Electromagnetic Transients ◽

Relativistic Hydrodynamic ◽

Hydrodynamic Simulations ◽

Relativistic Jet ◽

Nuclear Composition

ABSTRACT Neutron star mergers eject neutron-rich matter in which heavy elements are synthesized. The decay of these freshly synthesized elements powers electromagnetic transients (‘macronovae’ or ‘kilonovae’) whose luminosity and colour strongly depend on their nuclear composition. If the ejecta are very neutron-rich (electron fraction Ye < 0.25), they contain fair amounts of lanthanides and actinides that have large opacities and therefore efficiently trap the radiation inside the ejecta so that the emission peaks in the red part of the spectrum. Even small amounts of this high-opacity material can obscure emission from lower lying material and therefore act as a ‘lanthanide curtain’. Here, we investigate how a relativistic jet that punches through the ejecta can potentially push away a significant fraction of the high opacity material before the macronova begins to shine. We use the results of detailed neutrino-driven wind studies as initial conditions and explore with 3D special relativistic hydrodynamic simulations how jets are propagating through these winds. Subsequently, we perform Monte Carlo radiative transfer calculations to explore the resulting macronova emission. We find that the hole punched by the jet makes the macronova brighter and bluer for on-axis observers during the first few days of emission, and that more powerful jets have larger impacts on the macronova.

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Synthetic X-ray light curves of BL Lacs from relativistic hydrodynamic simulations

Astronomy and Astrophysics ◽

10.1051/0004-6361:20034261 ◽

2004 ◽

Vol 418 (3) ◽

pp. 947-958 ◽

Cited By ~ 35

Author(s):

P. Mimica ◽

M. A. Aloy ◽

E. Müller ◽

W. Brinkmann

Keyword(s):

Light Curves ◽

Relativistic Hydrodynamic ◽

Hydrodynamic Simulations ◽

X Ray ◽

Bl Lacs

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Quantiles as Robust Probes of Non-Gaussianity in 21-cm Images

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stab318 ◽

2021 ◽

Author(s):

Alon Banet ◽

Rennan Barkana ◽

Anastasia Fialkov ◽

Or Guttman

Keyword(s):

Galactic Halo ◽

Angular Resolution ◽

Research Effort ◽

First Stars ◽

X Ray ◽

Global Signal ◽

Radio Background ◽

Halo Masses ◽

The Universe ◽

Cosmic History

Abstract The epoch in which the first stars and galaxies formed is among the most exciting unexplored eras of the Universe. A major research effort is focused on probing this era with the 21-cm spectral line of hydrogen. While most research focuses on statistics like the 21-cm power spectrum or the sky-averaged global signal, there are other ways to analyze tomographic 21-cm maps, which may lead to novel insights. We suggest statistics based on quantiles as a method to probe non-Gaussianities of the 21-cm signal. We show that they can be used in particular to probe the variance, skewness, and kurtosis of the temperature distribution, but are more flexible and robust than these standard statistics. We test these statistics on a range of possible astrophysical models, including different galactic halo masses, star-formation efficiencies, and spectra of the X-ray heating sources, plus an exotic model with an excess early radio background. Simulating data with angular resolution and thermal noise as expected for the Square Kilometre Array (SKA), we conclude that these statistics can be measured out to redshifts above 20 and offer a promising statistical method for probing early cosmic history.

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The Voyage of Metals in the Universe from Cosmological to Planetary Scales: the need for a Very High-Resolution, High Throughput Soft X-ray Spectrometer

Experimental Astronomy ◽

10.1007/s10686-021-09710-2 ◽

2021 ◽

Author(s):

F. Nicastro ◽

J. Kaastra ◽

C. Argiroffi ◽

E. Behar ◽

S. Bianchi ◽

...

Keyword(s):

Chemical Composition ◽

High Resolution ◽

Deep Understanding ◽

High Resolution Spectroscopy ◽

X Ray ◽

Viable Solution ◽

Surrounding Space ◽

Nuclear Processes ◽

The Universe ◽

Very High

AbstractMetals form an essential part of the Universe at all scales. Without metals we would not exist, and the Universe would look completely different. Metals are primarily produced via nuclear processes in stars, and spread out through winds or explosions, which pollute the surrounding space. The wanderings of metals in-and-out of astronomical objects are crucial in determining their own evolution and thus that of the Universe as a whole. Detecting metals and assessing their relative and absolute abundances and energetics can thus be used to trace the evolution of these cosmic components. The scope of this paper is to highlight the most important open astrophysical problems that will be central in the next decades and for which a deep understanding of the Universe’s wandering metals, their physical and kinematical states, and their chemical composition represents the only viable solution. The majority of these studies can only be efficiently performed through High Resolution Spectroscopy in the soft X-ray band.

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A Highly Selective Turn-On Fluorescent Probe for the Detection of Zinc

Molecules ◽

10.3390/molecules26133825 ◽

2021 ◽

Vol 26 (13) ◽

pp. 3825

Author(s):

Ling-Yi Shen ◽

Xiao-Li Chen ◽

Xian-Jiong Yang ◽

Hong Xu ◽

Ya-Li Huang ◽

...

Keyword(s):

High Selectivity ◽

Fluorescence Probe ◽

Stoichiometric Ratio ◽

X Ray Diffraction ◽

X Ray ◽

Turn On ◽

Imine Nitrogen ◽

System A ◽

Plot Analysis ◽

L System

A novel turn-on fluorescence probe L has been designed that exhibits high selectivity and sensitivity with a detection limit of 9.53 × 10−8 mol/L for the quantification of Zn2+. 1H-NMR spectroscopy and single crystal X-ray diffraction analysis revealed the unsymmetrical nature of the structure of the Schiff base probe L. An emission titration experiment in the presence of different molar fractions of Zn2+ was used to perform a Job’s plot analysis. The results showed that the stoichiometric ratio of the complex formed by L and Zn2+ was 1:1. Moreover, the molecular structure of the mononuclear Cu complex reveals one ligand L coordinates with one Cu atom in the asymmetric unit. On adding CuCl2 to the ZnCl2/L system, a Cu-Zn complex was formed and a strong quenching behavior was observed, which inferred that the Cu2+ displaced Zn2+ to coordinate with the imine nitrogen atoms and hydroxyl oxygen atoms of probe L.

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The Hot Universe with XRISM and Athena

Proceedings of the International Astronomical Union ◽

10.1017/s1743921318007792 ◽

2018 ◽

Vol 14 (S342) ◽

pp. 29-36

Author(s):

M. Guainazzi ◽

M. S. Tashiro

Keyword(s):

Electromagnetic Radiation ◽

Large Scale ◽

Cosmological Evolution ◽

X Ray ◽

Hot Gas ◽

Cosmic Vision ◽

Esa Cosmic Vision ◽

The Universe

AbstractX-ray spectroscopy is key to address the theme of “The Hot Universe”, the still poorly understood astrophysical processes driving the cosmological evolution of the baryonic hot gas traceable through its electromagnetic radiation. Two future X-ray observatories: the JAXA-led XRISM (due to launch in the early 2020s), and the ESA Cosmic Vision L-class mission Athena (early 2030s) will provide breakthroughs in our understanding of how and when large-scale hot gas structures formed in the Universe, and in tracking their evolution from the formation epoch to the present day.

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Discovery of recombining plasma inside the extended gamma-ray supernova remnant HB9

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stz2461 ◽

2019 ◽

Vol 489 (3) ◽

pp. 4300-4310 ◽

Cited By ~ 5

Author(s):

A Sezer ◽

T Ergin ◽

R Yamazaki ◽

H Sano ◽

Y Fukui

Keyword(s):

Supernova Remnant ◽

Gamma Ray ◽

Radio Continuum ◽

Continuum Emission ◽

Large Area ◽

Imaging Spectrometer ◽

X Ray ◽

East Region ◽

X Ray Imaging ◽

Collisional Ionization

ABSTRACT We present the results from the Suzaku X-ray Imaging Spectrometer observation of the mixed-morphology supernova remnant (SNR) HB9 (G160.9+2.6). We discovered recombining plasma (RP) in the western Suzaku observation region and the spectra here are well described by a model having collisional ionization equilibrium (CIE) and RP components. On the other hand, the X-ray spectra from the eastern Suzaku observation region are best reproduced by the CIE and non-equilibrium ionization model. We discuss possible scenarios to explain the origin of the RP emission based on the observational properties and concluded that the rarefaction scenario is a possible explanation for the existence of RP. In addition, the gamma-ray emission morphology and spectrum within the energy range of 0.2–300 GeV are investigated using 10 yr of data from the Fermi Large Area Telescope (LAT). The gamma-ray morphology of HB9 is best described by the spatial template of radio continuum emission. The spectrum is well fit to a log-parabola function and its detection significance was found to be 25σ. Moreover, a new gamma-ray point source located just outside the south-east region of the SNR’s shell was detected with a significance of 6σ. We also investigated the archival H i and CO data and detected an expanding shell structure in the velocity range of $-10.5$ and $+1.8$ km s−1 that is coinciding with a region of gamma-ray enhancement at the southern rim of the HB9 shell.

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