Two-component Thermal Model Research Articles

Recombining Plasma and Gamma-Ray Emission in the Mixed-morphology Supernova Remnant 3C 400.2

Abstract 3C 400.2 belongs to the mixed-morphology supernova remnant class, showing center-filled X-ray and shell-like radio morphology. We present a study of 3C 400.2 with archival Suzaku and Fermi-LAT observations. We find recombining plasma (RP) in the Suzaku spectra of north–east and south–east regions. The spectra of these regions are well described by two-component thermal plasma models: the hard component is in RP, while the soft component is in collisional ionization equilibrium (CIE) conditions. The RP has enhanced abundances, indicating that the X-ray emission has an ejecta origin, while the CIE has solar abundances associated with the interstellar material. The X-ray spectra of north–west and south–west regions are best fitted by a two-component thermal plasma model: an ionizing and a CIE plasma. We have detected GeV gamma-ray emission from 3C 400.2 at the level of ∼5σ, assuming a point-like source model with a power-law (PL) type spectrum. We have also detected a new GeV source at the level of ∼13σ, assuming a Gaussian extension model with a PL-type spectrum in the neighborhood of the supernova remnant. We report the analysis results of 3C 400.2 and the new extended gamma-ray source, and discuss the nature of gamma-ray emission of 3C 400.2 in the context of existing NANTEN CO data, Dominion Radio Astrophysical Observatory H i data, and the Suzaku X-ray analysis results.

CHANDRAANDXMM-NEWTONSTUDY OF THE SUPERNOVA REMNANT KES 73 HOSTING THE MAGNETAR 1E 1841-045

We present a Chandra and XMM-Newton study of the supernova remnant (SNR) Kes 73 hosting the anomalous X-ray pulsar 1E 1841-045. The Chandra image reveals clumpy structures across the remnant with enhanced emission along the western rim. The X-ray emission fills the radio shell and spatially correlates with the infrared image. The global X-ray spectrum is described by a two-component thermal model with a column density N_H ~ 2.6e22 cm^{-2} and a total luminosity of L_X ~ 3.3e37 ergs/s (0.5-10 keV, at an assumed distance of 8.5 kpc). The soft component is characterized by a temperature kT_s ~ 0.5 keV, a high ionization timescale, and enhanced Si and S abundances suggesting emission that is dominated by shocked ejecta. The hard component has a temperature kT_h ~ 1.6 keV, a relatively low ionization timescale, and mostly solar abundances suggesting emission that is dominated by interstellar/circumstellar shocked material. A spatially resolved spectroscopy study reveals no significant variations in the spectral properties. We infer an SNR age ranging between 750 yr and 2100 yr, an explosion energy of ~0.3e51 ergs and a shock velocity of 1200 km/s (under the Sedov phase assumption). We also discuss the possible scenario for Kes 73 expanding into the late red supergiant wind phase of its massive progenitor. Comparing the inferred metal abundances to core-collapse nucleosynthesis model yields, we estimate a progenitor mass >20 solar masses, adding a candidate to the growing list of highly magnetized neutron stars proposed to be associated with very massive progenitors.

X-ray imaging and spectroscopic study of the SNR Kes 73 hosting the magnetar 1E 1841–045

AbstractWe present the first detailed Chandra and XMM-Newton study of the young Galactic supernova remnant (SNR) Kes 73 associated with the anomalous X-ray pulsar (AXP) 1E 1841–045. Images of the remnant in the radio (20 cm), infrared (24 μm), and X-rays (0.5–7 keV) reveal a spherical morphology with a bright western limb. High-resolution Chandra images show bright diffuse emission across the remnant, with several small-scale clumpy and knotty structures filling the SNR interior. The overall Chandra and XMM-Newton spectrum of the SNR is best described by a two-component thermal model with the hard component characterized by a low ionization timescale, suggesting that the hot plasma has not yet reached ionization equilibrium. The soft component is characterized by enhanced metal abundances from Mg, Si, and S, suggesting the presence of metal-rich supernova ejecta. We discuss the explosion properties of the supernova and infer the mass of its progenitor star. Such studies shed light on our understanding of SNRs associated with highly magnetized neutron stars.

Hot and cool: two emission-line stars with constrasting behaviours in the same XMM-Newtonfield

High-energy emissions are good indicators of peculiar behaviours in stars. We have therefore obtained an XMM-Newton observation of HD155806 and 1RXSJ171502.4-333344, and derived their spectral properties for the first time. The X-ray spectrum of HD155806 appears soft, even slightly softer than usual for O-type stars (as shown by a comparison with the O9 star HD155889 in the same XMM field). It is well-fitted with a two-component thermal model with low temperatures (0.2 and 0.6 keV), and it shows no overluminosity (log[LX/Lbol]=-6.75). The high-resolution spectrum, though noisy, reveals a few broad, symmetric X-ray lines (FWHM ~ 2500 km/s). The X-ray emission is compatible with the wind-shock model and therefore appears unaffected by the putative dense equatorial regions at the origin of the Oe classification. 1RXSJ171502.4-333344 is a nearby flaring source of moderate X-ray luminosity (log[LX/Lbol]=-3), with a soft thermal spectrum composed of narrow lines and presenting a larger abundance of elements (e.g. Ne) with a high first ionization potential (FIP) compared to lower-FIP elements. All the evidence indicates a coronal origin for the X-ray emission, in agreement with the dMe classification of this source.

Observations of X‐Rays and Thermal Dust Emission from the Supernova Remnant Kes 75

We present Spitzer Space Telescope and Chandra X-ray Observatory observations of the composite Galactic supernova remnant Kes 75 (G29.7-0.3). We use the detected flux at 24 microns and hot gas parameters from fitting spectra from new, deep X-ray observations to constrain models of dust emission, obtaining a dust-to-gas mass ratio M_dust/M_gas ~0.001. We find that a two-component thermal model, nominally representing shocked swept-up interstellar or circumstellar material and reverse-shocked ejecta, adequately fits the X-ray spectrum, albeit with somewhat high implied densities for both components. We surmise that this model implies a Wolf-Rayet progenitor for the remnant. We also present infrared flux upper limits for the central pulsar wind nebula.

The analysis of Abell 1835 using a deprojection technique

We present the results from a detailed deprojection analysis of Abell 1835 as observed by {\it XMM-Newton}. If we fit the spectra with an isothermal plasma model, the deprojected temperature profile is flat in the outer region around 7.6 keV and decreases to $\sim$ 5.6 keV in the center, which may be connected with the gas cooling. In the central part, a two-component thermal plasma model can fit the spectrum significantly better. Moreover, the cool component (T $\sim$ 1.8 keV) has a much lower metal abundance than the hot component (T $\sim$ 8 keV), which may be due to the longer cooling time for the cool gas with lower abundance. In addition, it was found that without a main isothermal component, the standard cooling flow model cannot fit the spectrum satisfactorily. From the isothermal model fitting results we also derived the electron density $n_e$, and fitted its radial distribution with a double-$\beta$ model. The $n_e$ profile inferred with the double-$\beta$ model and the deprojected X-ray gas temperature profile were then combined to derive the total mass and the total projected mass of the cluster. The projected mass is lower than that derived from the weak lensing method. However, assuming that the cluster extends to a larger radius $\sim15'$ as found by Clowe & Schneider (2002), the two results are consistent within the error bars. Furthermore, we calculated the projected mass within the radius of $\sim$ 153 kpc implied by the presence of a gravitational lensing arc, which is about half of the mass determined from the optical lensing.

The X‐Ray–faint Early‐Type Galaxy NGC 4697

We analyze archival ROSAT HRI, ROSAT PSPC, and ASCA data of the X-ray faint early-type galaxy NGC4697. The joint ROSAT PSPC + ASCA spectrum is fit by a two-component thermal model, a MEKAL model with kT_{MEKAL}=0.26^{+0.04}_{-0.03} keV with low metallicity and a bremsstrahlung model with kT_{BREM}=5.2^{+3.0}_{-1.6} keV. A similar model was found to fit the spectra of another faint early-type galaxy (NGC4382) and the bulge of M31. We interpret this soft emission as a combination of emission from a soft component of low mass X-ray binaries (LMXBs) and from a low temperature interstellar medium, although the relative contributions of the two components could not be determined. Twelve point sources were identified within 4' of NGC4697, of which 11 are most likely LMXBs associated with the galaxy. The soft X-ray colors of four of the LMXBs in NGC4697 support the claim that LMXBs possess a soft spectral component. Finally, we present a simulation of what we believe the Chandra data of NGC4697 will look like.

Centrality dependence of pion and proton spectra in C+C and C+Ta interactions at 4.2 GeV/c per nucleon.

Target and centrality dependence of pion and proton distributions is studied in C+C and C+Ta collisions at 4.2 GeV/c per nucleon using the 2-m propane bubble chamber. The experimental data are compared with the predictions of the Monte Carlo quark-gluon string model (QGSM). The pion and proton transverse momentum spectra at midrapidity are well described by the two-component thermal model. The shape of the proton rapidity distribution strongly depends on the collision centrality and reflects the stopping power of colliding nuclei. The pion rapidity distribution is Gaussian in shape regardless of the target mass number and collision centrality. The QGSM completely reproduces main features of pion and proton rapidity spectra as well as pion transverse momentum spectra. The model does not fully reproduce the features of the proton transverse momentum spectra.

Temperature of an active lava channel from spectral measurements, Kilauea Volcano, Hawaii

A narrow band spectroradiometer was used to determine the characteristic temperatures of a very active channeled lava flow for the phase 50 eruption of Pu'u 'O'o on the East Rift Zone of Kilauea Volcano, Hawaii. During the twilight of 19 February 1992, 14 spectra of this activity were acquired over a 51 minute interval [18.29 to 19.20 Hawaiian Standard Time (HST)], from which the thermal distribution of energy of two 18 m2 areas, one near the center and one near the margin of the flow, may be investigated. A twocomponent thermal mixing model applied to the data taken of the center of the channel gave, in the most powerful instance (1.8x105 W/m2), a crust temperature of 940° C, a hot component temperature of 1120°C and a hot radiating area of 60% of the total area. A simultaneous spectrum acquired near the channeled flow margin yielded a crust temperature of 586° C and a hot area of only 1.2% of the total area radiating at 1130° C. Average radiant flux densities recorded for the center of the lava channel (1.3x105 W/m2 average) are much greater than previous measurements of lava lakes (4.9x103 W/m2) or recently emplaced lava flows (maximum of 7.2x104 W/m2). The energetic nature of this eruption is shown by satellite measurements made at 02.33 HST on 22 February 1992 by the Advanced Very High Resolution Radiometer in Band 2 (0.72–1.10 μm). These show the utility of using existing satellites with moderate resolution (1 km x 1 km pixels) and high temporal coverage (eight overpasses each day for Hawaii) as potential thermal alarms for rapidly assessing the hazard potential of large volcanic eruptions.

ROSAT PSPC observations of two X-ray-faint early-type galaxies: NGC 4365 and NGC 4382

view Abstract Citations (74) References (33) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS ROSAT PSPC Observations of Two X-Ray--faint Early-Type Galaxies: NGC 4365 and NGC 4382 Fabbiano, G. ; Kim, D. -W. ; Trinchieri, G. Abstract We present the results of ROSAT PSPC observations of the two early- type galaxies NGC 4365 and NGC 4382. These galaxies are among those observed with Einstein to have the lowest X-ray to optical flux ratios of early-type galaxies. The PSPC data show that for radii r > 50" the radial distributions of the X-ray surface brightness are consistent with the optical distributions of King (1978). We also find that these galaxies have X-ray spectra significantly different from those observed in X-ray- bright ellipticals, with a relative excess of counts detected in the softest spectral channels. This confirms earlier Einstein results. The characteristics of the ROSAT PSPC do not allow us to discriminate between possible spectral models. If we adopt a two-component thermal model on the grounds of physical plausibility, we find that the spectral data can be fitted with a very soft optically thin component, with kT ~ 0.2 kev, and a hard component with kT > (1.0-1.5) keV. The hard component has a luminosity consistent with that expected from the integrated emission of a population of low-mass X-ray binaries in these galaxies; the nature of the very soft component is more speculative. Candidates include the coronal emission of late-type stars, supersoft X-ray sources, RS CVn, and perhaps a hot ISM. Alternatively, the spectral data may be fitted with a 0.6-1 keV bremsstrahlung spectrum (exponential plus Gaunt), and may suggest the presence of a totally new population of X-ray sources. Publication: The Astrophysical Journal Pub Date: July 1994 DOI: 10.1086/174304 Bibcode: 1994ApJ...429...94F Keywords: Early Stars; Galactic Radiation; Light Emission; Radiative Transfer; X Ray Sources; Astronomical Models; Bremsstrahlung; Elliptical Galaxies; Lenticular Bodies; Rosat Mission; X Ray Binaries; Astrophysics; GALAXIES: ELLIPTICAL AND LENTICULAR; CD; GALAXIES: INDIVIDUAL NGC NUMBER: NGC 4365; GALAXIES: INDIVIDUAL NGC NUMBER: NGC 4382; RADIATION MECHANISMS: NONTHERMAL; RADIATION MECHANISMS: THERMAL; X-RAYS: GALAXIES full text sources ADS | data products SIMBAD (2) NED (2) HEASARC (1)

Cooling rate of an active Hawaiian lava flow from nighttime spectroradiometer measurements

A narrow‐band spectroradiometer has been used to make nighttime measurements of the Phase 50 eruption of Pu'u O'o, on the East Rift Zone of Kilauea Volcano, Hawaii. On February 19, 1992, a GER spectroradiometer was used to determine the cooling rate of an active lava flow. This instrument collects 12‐bit data between 0.35 to 3.0 μm at a spectral resolution of 1 – 5 nm. Thirteen spectra of a single area on a pahoehoe flow field were collected over a 59 minute period (21:27 – 22:26 HST) from which the cooling of the lava surface has been investigated. A two‐component thermal mixing model [Flynn, 1992] applied to data for the flow immediately on emplacement gave a best‐fit crustal temperature of 768°C, a hot component at 1150°C, and a hot radiating area of 3.6% of the total area. Over a 52‐minute period (within the time interval between flow resurfacings) the lava flow crust cooled by 358°C to 410°C at a rate that was as high as 15°C min−1. Our observations have significance both for satellite observations of active volcanoes and for numerical models of the cooling of lava flows during their emplacement.

The heliocentric evolution of cometary infrared spectra: Results from an organic grain model

Observations of Comets Halley and Wilson reveal an emission feature peaking near 3.4 μm, characteristic of C-H stretching in hydrocarbons. We have previously (Chyba and Sagan 1987a, Nature (London) 330, 350–353) fit this feature with a simple two-component thermal emission model for dust in the cometary coma (one component corresponding to large, cool, optically thick particles, the other due to smaller, hotter, organic grains) by employing laboratory spectra of the organic residue produced by the irradiation of carbon-bearing ices. This procedure yields optical depths in agreement with limits from spacecraft data. One remarkable result of such modeling is that at ∼1 AU emission features at wavelengths longer than 3.4 μm are largely overwhelmed (or “diluted”) by continuum emission. The large particle optical depth is ∼10 2 times that of the emitting organics, so that, relative to the continuum, only near the continuum minimum can the emitting organics make a significant contribution. At ∼1 AU, the 3.4-μm feature is the sole feature near that minimum, lying at the intersection of the curves for particle thermal emission and scattered sunlight. Thus, since as a comet moves away from perhelion the intersection of the scattered solar spectrum and the comet's thermal emission spectrum will move to longer wavelengths, we predicted (Chyba and Sagan 1987a) that the 3.4-μm feature is diluted while those at longer wavelengths are progressively revealed—so long as the comet retains its coma. We now quantitatively develop this model and find agreement with observational data for Comet Halley for certain plausible values of optical constants. Thus the observed heliocentric evolution of the 3.4-μm feature provides information on the composition, and perhaps structure, of the organic grains in Comet Halley. In addition, we argue that the heliocentric evolution of organic features will differ in the cases of thermal emission from small grains and gas-phase fluorescence. Therefore observations of cometary spectral evolution can in principle distinguish between solid or gas-phase origins for these features.

Infrared emission by organic grains in the coma of comet Halley

Spacecraft1 and ground-based2–5 observations of comet Halley in the near-infrared reveal a triple-peaked emission feature near 3.4 µm, characteristic of C–H stretching in hydrocarbons (–CH3 and –CH2– alkanes). Here we discuss transmission spectra of organic residues produced by laboratory irradiation of candidate cometary ices, which serve as the basis for a model of emitting cometary dust. The laboratory synthesis of solid organic residue from irradiated low-occupancy methane ice clathrate simulates the radiation processing experienced by comet Halley. The transmission spectrum of this residue, convolved with a simple two-component thermal emission model based on the spacecraft-determined dust distribution in the Halley coma, fits the 3.4 µm feature, provides optical depths in excellent agreement with those observationally determined, and accounts for the absence of features at longer wavelengths (despite their presence in transmission spectra of typical ice irradiation residues).

A two-component thermal model for a direct gain passive house with a heated basement

A model of a direct gain passive house with a heated basement was developed. This model predicts the room temperature and the heat requirement of houses as a function of meteorological variables and the design parameters. The key concept introduced to develop this model is that the basement heat loss can be divided into two components: one with an annual variation and one with a diurnal variation. The impact of these two components on the heat requirement of a house is analysed. The results are in good agreement with the experimental data as to the combined effects of the house heat loss rate, the thermal mass, and the solar gains. Of particular interest to house heating is the result that the basement walls in a passive house could contribute significantly to the thermal mass of the house.

Temperature structure in the lower atmosphere of Venus: New results derived from pioneer Venus entry probe measurements

The interpretation of unexpected characteristics of Pioneer Venus temperature measurements, and of the large difference between these and the Venera results, is aided by new Venus temperature profiles derived from engineering measurements of the Pioneer Venus Small-Probe Net Flux Radiometer (SNFR) instruments. To facilitate correction of a temperature-dependent radiometric response, these instruments monitored the temperatures of their deployed radiation detectors. The accurate calibration of the temperature sensors, and their strong thermal coupling to the atmosphere, make it possible to deduce atmospheric temperatures within 2°K (at most altitudes) using a simple two-component thermal model to account for lag effects. These independent temperature profiles generally confirm to high accuracy, the small-probe results of A. Seiff, D. B. Kirk, R. E. Young, R. C. Blanchard, J. T. Findlay, G. M. Kelly, and S. C. Sommer (1980a, J. Geophys. Res. 85, pp. 7903–7933) concerning vertical structure and horizontal contrast in the lower atmosphere, although the stable layer below 25 km is found to be slightly more stable (by about 0.4°K/km) and absolute temperatures are an average of 2°K higher. The measured Day-Night thermal contrast is compatible with predicted responses to the diurnal variation in solar heating, except near the cloud base, where 3–5°K differences may be due to thermal radiative heating differences associated with different cloud opacities. Temperature contrasts between latitudes 30 and 60° are roughly consistent with cyclostrophic balance. But pressure and temperature measurements by the Pioneer Venus Sounder probe at 4° latitude, when compared to Small-probe results, imply unreasonably large equatorward accelerations of 100 (m/sec)/day. Poleward accelerations compatible with cyclostrophic balance can be obtained if Sounder-probe temperatures are increased by a scale-factor correction reaching 6–7°K at 13 km.

X-ray observations of Algol

The Solid State Spectrometer on Einstein has been used to study Algol. Two observations six months apart were made, both including a primary optical eclipse. No corresponding X-ray eclipses were seen. During the second observation the source was flaring and was on the average a factor of three brighter. The spectrum on both occasions was consistent with a two-component thermal equilibrium model with temperatures of approximately 7.5 and 40 million degrees. Attempts to insert a third component indicate the temperature distribution to be bimodal. Models for the X-ray emission are discussed and it is suggested that it most likely originates from an active corona surrounding the K star.

A two-component thermal model of X-ray burst sources

A semi-empirical model of the soft X-ray source associated with solar flares is presented, based on the results of the two temperature analysis of OSO-5 data obtained by Herring and Craig (1973). The model makes use of a jet of plasma rising from the solar surface as the basic origin of the soft X-ray emitting region, and gives rise to a cool region caused by randomisation of the jet, and a hot region caused by a shock front. Two different geometries are examined, and the model allows flow velocities and electron densities to be calculated.