A Solar Magnetic-fan Flaring Arch Heated by Nonthermal Particles and Hot Plasma from an X-Ray Jet Eruption

A program is under way to develop methods and instrumentation based on charge-coupled device (CCD) sensors for hot plasma diagnostics. We have developed a new X-ray spectrometer in which a freestanding X-ray transmission grating is coupled to a CCD linear array detector with electronic digitized readout replacing film and its wet processing. This instrument measures time-integrated pulsed X-ray spectra with moderate spectral resolution (δλ ≤ 0.6 nm) over a broad spectral range (0.3–2 keV) with high sensitivity, linearity, and large dynamic range. The performance of the device was tested using laser plasma as the X-ray source.

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SolpeX: the soft X-ray flare polarimeter–spectrometer for the ISS

Proceedings of the International Astronomical Union ◽

10.1017/s1743921315004627 ◽

2014 ◽

Vol 10 (S305) ◽

pp. 114-120

Author(s):

Janusz Sylwester ◽

Stefan Płocieniak ◽

Jarosław Bakała ◽

Żaneta Szaforz ◽

Marek Stȩślicki ◽

...

Keyword(s):

Solar Flares ◽

Line Emission ◽

Impulsive Phase ◽

Particle Beams ◽

X Ray ◽

Hot Plasma ◽

Spectral Imager ◽

Polarized Bremsstrahlung ◽

Made In ◽

Fast Rotating

AbstractWe present the innovative soft X-ray spectro-polarimeter, SolpeX. This instrument consists of three functionally independent blocks. They are to be included into the Russian instrument KORTES, to be mounted onboard the ISS. The three SolpeX units are: a simple pin-hole X-ray spectral imager, a polarimeter, and a fast-rotating drum multiple-flat-crystal Bragg spectrometer. Such a combination of measuring blocks will offer a new opportunity to reliably measure possible X-ray polarization and spectra of solar flares, in particular during the impulsive phase. Polarized Bremsstrahlung and line emission due to the presence of directed particle beams will be detected, and measurements of the velocities of evaporated hot plasma will be made. In this paper we discuss the details of the construction of the SolpeX units. The delivery of KORTES with SolpeX to the ISS is expected to happen in 2017/2018.

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Expansion of hot plasma with Kappa distribution in coronal flare sources

10.5194/egusphere-egu21-11962 ◽

2021 ◽

Author(s):

Jan Benáček ◽

Marian Karlický

Keyword(s):

Langmuir Wave ◽

Maxwellian Distribution ◽

Double Layers ◽

Kappa Distribution ◽

One Dimensional ◽

X Ray ◽

Particle In Cell ◽

Hot Plasma ◽

The Difference ◽

Field Lines

<p>We study how hot plasma that is released during a solar flare can be confined in its source and interact with surrounding colder plasma. The X-ray emission of coronal flare sources is well explained using Kappa velocity distribution. Therefore, we compare the difference in the confinement of plasma with Kappa and Maxwellian distribution. We use a 3D Particle-in-Cell code, which is large along magnetic field lines, effectively one-dimensional, but contains all electromagnetic effects. In the case with Kappa distribution, contrary to Maxwellian distribution, we found formation of several thermal fronts associated with double-layers that suppress particle fluxes. As the Kappa distribution of electrons forms an extended tail, more electrons are not confined by the first front and cause formation of multiple fronts. A beam of electrons from the hot part is formed at each front; it generates return current, Langmuir wave density depressions, and a double layer with a higher potential step than in the Maxwellian case. We compare the Kappa and Maxwellian cases and discuss how these processes could be observed.</p>

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X-Ray Flares and Outflows Driven by Magnetic Interaction Between a Protostar and its Surrounding Disk

International Astronomical Union Colloquium ◽

10.1017/s0252921100043608 ◽

1997 ◽

Vol 163 ◽

pp. 717-718

Author(s):

Mitsuru Hayashi ◽

Kazunari Shibata ◽

Ryoji Matsumoto

Keyword(s):

Magnetic Field ◽

Current Sheet ◽

Plasma Temperature ◽

Magnetic Interaction ◽

Central Star ◽

X Ray ◽

Mhd Simulations ◽

Flare Loops ◽

Hot Plasma ◽

Dipole Magnetic Field

AbstractHere we present a model of hard X-ray flares and hot plasma outflows (optical jets) observed in protostars. Assuming that the dipole magnetic field of a protostar threads the protostellar disk, we carried out 2.5-dimensional magnetohydrodynamic (MHD) simulations of the diskstar interaction. The closed magnetic loops connecting the central star and the disk are twisted by the rotation of the disk. In the presence of resistivity, magnetic reconnection takes place in the current sheet formed inside the expanding loops. Hot, outgoing plasmoid and post flare loops are formed as a result of the reconnection. Numerical results are consistent with the observed plasma temperature (107 – 108K), the length of the flaring loop (1011 – 1012cm), and the speed of optical jets (200 – 400 km s−1 ).

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The Nature of the Compact Object in the Hard X-Ray Source 4U2206+54

International Astronomical Union Colloquium ◽

10.1017/s0252921100152546 ◽

2004 ◽

Vol 194 ◽

pp. 208-208

Author(s):

J. M. Torrejón ◽

I. Kreykenbohni ◽

A. Orr ◽

L. Titarchuk ◽

I. Negueruela

Keyword(s):

Neutron Star ◽

Accretion Disk ◽

Compact Object ◽

High Energy ◽

Energy Data ◽

X Ray ◽

Hot Plasma ◽

Cyclotron Line ◽

First Time

We present an analysis of archival RXTE and BeppoSAX data of the X-ray source 4U2206+54. For the first time, high energy data (≥ 30 keV) is analyzed. The data is well described by comptonization models in which seed photons with temperatures between 1.1 keV arid 1.5 keV are comptonized by a hot plasma at 50 keV thereby producing a hard tail which extends up to 100 keV. From luminosity arguments it is shown that the area of the soft photons source must be small (r ≈ 1 km) and that the presence of an accretion disk in this system is unlikely. Here we report on the possible existence of a cyclotron line around 30 keV . The presence of a neutron star in the system is strongly favored by the available data.

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Mixed-morphology supernova remnants: the case of SNR 0520–69.4 in the Large Magellanic Cloud

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa3138 ◽

2020 ◽

Vol 499 (3) ◽

pp. 4213-4222

Author(s):

I Ramírez-Ballinas ◽

J Reyes-Iturbide ◽

P Ambrocio-Cruz ◽

R Gabbasov ◽

M Rosado

Keyword(s):

Supernova Remnants ◽

Plasma Temperature ◽

Optical Emission ◽

Large Magellanic Cloud ◽

Magellanic Cloud ◽

Physical Parameters ◽

X Ray ◽

Hot Plasma ◽

Observatory Data ◽

Fabry Perot

ABSTRACT We present observations in X-ray and optical emission of the supernova remnant (SNR) 0520–69.4 in the Large Magellanic Cloud. Using XMM–Newton observatory data, we produced images of the diffuse X-ray emission and spectra to obtain the X-ray parameters, such as luminosity and temperature, of hot plasma in the SNR. Diffuse X-ray emission with filled-centre morphology goes beyond the Hα region, suggesting that the hot gas escapes through the pores of the Hα shell. We fitted a model that has a plasma temperature of 1.1 × 107 K for an X-ray thermal luminosity of 3.3 × 1035 erg s−1. However, from Hα and [O iii] Fabry–Perot observations obtained with the Marseille Hα Survey of the Magellanic Clouds and the Milky Way at La Silla, European Southern Observatory, we are able to obtain physical parameters such as the velocity of the shock induced in the cloudlets emitting at optical wavelengths and the electron density of this gas. With the parameters described above, we test the model proposed by White & Long (1991, ApJ, 373, 543) for explaining the mixed-morphology observed.

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The Soft X-ray Background Spectrum from DXS

International Astronomical Union Colloquium ◽

10.1017/s0252921100070779 ◽

1997 ◽

Vol 166 ◽

pp. 83-90 ◽

Cited By ~ 1

Author(s):

W.T. Sanders ◽

R.J. Edgar ◽

D.A. Liedahl ◽

J.P. Morgenthaler

Keyword(s):

Galactic Plane ◽

Emission Lines ◽

Background Spectrum ◽

Local Bubble ◽

X Ray ◽

Hot Plasma ◽

Solar Abundances ◽

Ionic Emission ◽

X Ray Background ◽

Ionization Balance

AbstractThe Diffuse X-ray Spectrometer (DXS) obtained spectra of the low energy X-ray (44 – 83 Å) diffuse background near the galactic plane from galactic longitudes 150° ≲ l ≲ 300° with ≲ 3 Å spectral resolution and ~ 15° angular resolution. Thus, DXS measured X-ray spectra that arise almost entirely from within the Local Bubble. The DXS spectra show emission lines and emission-line blends, indicating that the source of the X-ray emission is thermal – hot plasma in the Local Bubble. The measured spectra are not consistent with those predicted by standard coronal models, either with solar abundances or depleted abundances, over the temperature range 105 – 107 K. The measured spectra are also inconsistent with the predictions of various non-equilibrium models. A nearly acceptable fit to DXS spectra can be achieved using a hybrid model that combines the Raymond & Smith ionization balance calculation with recently calculated (by DAL) ionic emission lines.

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Magnetic Reconnection as the Origin of Galactic Ridge X-Ray Emission

Symposium - International Astronomical Union ◽

10.1017/s0074180900115086 ◽

1998 ◽

Vol 188 ◽

pp. 269-270 ◽

Cited By ~ 1

Author(s):

S. Tanuma ◽

T. Yokoyama ◽

T. Kudoh ◽

K. Shibata ◽

R. Matsumoto ◽

...

Keyword(s):

Magnetic Field ◽

Magnetic Reconnection ◽

Galactic Plane ◽

Thermal Emission ◽

Mhd Equations ◽

Magnetic Islands ◽

Cool Component ◽

X Ray ◽

Hot Plasma ◽

Helical Tubes

We present a scenario for the origin of the hot plasma in our Galaxy, as a model of a strong X-ray emission (LX(2 – 10keV) ~ 1038 erg s−1), called Galactic Ridge X-ray Emission (GRXE), which has been observed near the Galactic plane. GRXE is thermal emission from hot component (~ 7 keV) and cool component (~ 0.8 keV). Observations suggest that the hot component is diffuse, and is not escaping away freely. Both what heats the hot component and what confines it in the Galactic ridge are still remained puzzling, while the cool component is believed to be made by supernovae. We propose a new scenario: the hot component of GRXE plasma is heated by magnetic reconnection, and confined in the helical magnetic field produced by magnetic reconnection or in the current sheet and magnetic field. We solved also the 2-dimensional magnetohydrodynamic (MHD) equations numerically to study how the magnetic reconnection creates hot plasmas and magnetic islands (helical tubes), and how the magnetic islands confine the hot plasmas in Galaxy. We conclude that the magnetic reconnection is able to heat up the cool component to hot component of GRXE plasma if the magnetic field is localized into intense flux tube with Blocal ~ 30 μG (the volume filling factor of f ~ 0.1).

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X-ray Emission from Massive Stars at the Core of Very Young Clusters

Proceedings of the International Astronomical Union ◽

10.1017/s1743921317003532 ◽

2016 ◽

Vol 12 (S329) ◽

pp. 362-365

Author(s):

Norbert S. Schulz

Keyword(s):

Massive Stars ◽

Stellar Winds ◽

X Rays ◽

Stellar Clusters ◽

Orion Nebula ◽

X Ray ◽

The Core ◽

Hot Plasma ◽

Young Clusters ◽

Massive Cluster

AbstractMost cores of very young stellar clusters contain one or more massive stars at various evolutionary stages. Observations of the Orion Nebula Cluster, Trumpler 37, NGC 2362, RCW38, NGC 3603 and many others provide the most comprehensive database to study stellar wind properties of these massive cluster stars in X-rays. In this presentation we review some of these observations and results and discuss them in the context of stellar winds and possible evolutionary implications. We argue that in very young clusters such as RCW38 and M17, shock heated remnants of a natal shell could serve as an alternate explanation to the colliding wind paradigm for the hot plasma components in the X-ray spectra.

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