scholarly journals Quiescent Prominences in the Era of ALMA. II. Kinetic Temperature Diagnostics

2018 ◽  
Vol 853 (1) ◽  
pp. 21 ◽  
Author(s):  
Stanislav Gunár ◽  
Petr Heinzel ◽  
Ulrich Anzer ◽  
Duncan H. Mackay
Keyword(s):  
Kinetic Temperature ◽  
Temperature Diagnostics

Temperature Diagnostics for Field-Reversed Configuration Plasmas on the Pulsed High Density (PHD) Experiment

2007 ◽  
Vol 2 ◽  
pp. S1050-S1050
Author(s):  
Hiroshi GOTA ◽  
Samuel ANDREASON ◽  
George VOTROUBEK ◽  
Chris PIHL ◽  
John SLOUGH
Keyword(s):  
High Density ◽  
Field Reversed Configuration ◽  
Temperature Diagnostics

scholarly journals Active matter at high density: Velocity distribution and kinetic temperature

2020 ◽  
Vol 153 (18) ◽  
pp. 184901
Author(s):  
Lorenzo Caprini ◽  
Umberto Marini Bettolo Marconi
Keyword(s):  
Velocity Distribution ◽  
High Density ◽  
Kinetic Temperature ◽  
Active Matter

Use of γ-ray-generating nuclear reactions for temperature diagnostics of DT fusion plasma

2001 ◽  
Vol 63 (2) ◽  
Author(s):  
V. T. Voronchev ◽  
V. I. Kukulin ◽  
Y. Nakao
Keyword(s):  
Nuclear Reactions ◽  
Fusion Plasma ◽  
Temperature Diagnostics ◽  
Γ Ray

scholarly journals The kinetic temperature of a molecular cloud at redshift 0.9: ammonia in the gravitational lens PKS 1830–211

2008 ◽  
Vol 485 (2) ◽  
pp. 451-456 ◽  
Author(s):  
C. Henkel ◽  
J. A. Braatz ◽  
K. M. Menten ◽  
J. Ott
Keyword(s):  
Molecular Cloud ◽  
Gravitational Lens ◽  
Kinetic Temperature

scholarly journals Molecular gas in the Herschel-selected strongly lensed submillimeter galaxies at z ~ 2–4 as probed by multi-J CO lines

2017 ◽  
Vol 608 ◽  
pp. A144 ◽  
Author(s):  
C. Yang ◽  
A. Omont ◽  
A. Beelen ◽  
Y. Gao ◽  
P. van der Werf ◽  
...  
Keyword(s):  
Star Formation ◽  
High Redshift ◽  
Line Emission ◽  
Far Infrared ◽  
Molecular Gas ◽  
Kinetic Temperature ◽  
Large Area ◽  
Line Energy ◽  
Submillimeter Galaxies ◽  
Dust Mass

We present the IRAM-30 m observations of multiple-J CO (Jup mostly from 3 up to 8) and [C I](3P2 → 3P1) ([C I](2–1) hereafter) line emission in a sample of redshift ~2–4 submillimeter galaxies (SMGs). These SMGs are selected among the brightest-lensed galaxies discovered in the Herschel-Astrophysical Terahertz Large Area Survey (H-ATLAS). Forty-seven CO lines and 7 [C I](2–1) lines have been detected in 15 lensed SMGs. A non-negligible effect of differential lensing is found for the CO emission lines, which could have caused significant underestimations of the linewidths, and hence of the dynamical masses. The CO spectral line energy distributions (SLEDs), peaking around Jup ~ 5–7, are found to be similar to those of the local starburst-dominated ultra-luminous infrared galaxies and of the previously studied SMGs. After correcting for lensing amplification, we derived the global properties of the bulk of molecular gas in the SMGs using non-LTE radiative transfer modelling, such as the molecular gas density nH2 ~ 102.5–104.1 cm-3 and the kinetic temperature Tk  ~ 20–750 K. The gas thermal pressure Pth ranging from~105 K cm-3 to 106 K cm-3 is found to be correlated with star formation efficiency. Further decomposing the CO SLEDs into two excitation components, we find a low-excitation component with nH2 ~ 102.8–104.6 cm-3 and Tk  ~ 20–30 K, which is less correlated with star formation, and a high-excitation one (nH2 ~ 102.7–104.2 cm-3, Tk  ~ 60–400 K) which is tightly related to the on-going star-forming activity. Additionally, tight linear correlations between the far-infrared and CO line luminosities have been confirmed for the Jup ≥ 5 CO lines of these SMGs, implying that these CO lines are good tracers of star formation. The [C I](2–1) lines follow the tight linear correlation between the luminosities of the [C I](2–1) and the CO(1–0) line found in local starbursts, indicating that [C I] lines could serve as good total molecular gas mass tracers for high-redshift SMGs as well. The total mass of the molecular gas reservoir, (1–30) × 1010M⊙, derived based on the CO(3–2) fluxes and αCO(1–0) = 0.8 M⊙ ( K km s-1 pc2)-1, suggests a typical molecular gas depletion time tdep ~ 20–100 Myr and a gas to dust mass ratio δGDR ~ 30–100 with ~20%–60% uncertainty for the SMGs. The ratio between CO line luminosity and the dust mass L′CO/Mdust appears to be slowly increasing with redshift for high-redshift SMGs, which need to be further confirmed by a more complete SMG sample at various redshifts. Finally, through comparing the linewidth of CO and H2O lines, we find that they agree well in almost all our SMGs, confirming that the emitting regions of the CO and H2O lines are co-spatially located.

Coronal temperature diagnostics from high-resolution soft X-ray spectra

1988 ◽  
Vol 8 (11) ◽  
pp. 167-171 ◽  
Author(s):  
K.T. Strong ◽  
E.S. Claflin ◽  
J.R. Lemen ◽  
G.A. Linford
Keyword(s):  
High Resolution ◽  
Coronal Temperature ◽  
X Ray ◽  
Temperature Diagnostics

scholarly journals L1495 revisited: a ppmap view of a star-forming filament

2019 ◽  
Vol 489 (1) ◽  
pp. 962-976 ◽  
Author(s):  
A D P Howard ◽  
A P Whitworth ◽  
K A Marsh ◽  
S D Clarke ◽  
M J Griffin ◽  
...  
Keyword(s):  
Critical Line ◽  
Kinetic Temperature ◽  
Line Density ◽  
Star Forming ◽  
Physical Conditions ◽  
Fitting Procedure ◽  
Different Types ◽  
Prestellar Cores ◽  
Different Temperatures ◽  
Average Profile

ABSTRACT We have analysed the Herschel and SCUBA-2 dust continuum observations of the main filament in the Taurus L1495 star-forming region, using the Bayesian fitting procedure ppmap. (i) If we construct an average profile along the whole length of the filament, it has FWHM $\simeq 0.087\pm 0.003\, {\rm pc};\,\,$ but the closeness to previous estimates is coincidental. (ii) If we analyse small local sections of the filament, the column-density profile approximates well to the form predicted for hydrostatic equilibrium of an isothermal cylinder. (iii) The ability of ppmap to distinguish dust emitting at different temperatures, and thereby to discriminate between the warm outer layers of the filament and the cold inner layers near the spine, leads to a significant reduction in the surface-density, $\varSigma$, and hence in the line-density, μ. If we adopt the canonical value for the critical line-density at a gas-kinetic temperature of $10\, {\rm K}$, $\mu _{{\rm CRIT}}\simeq 16\, {\rm M_{\odot }\, pc^{-1}}$, the filament is on average trans-critical, with ${\bar{\mu }}\sim \mu _{{\rm CRIT}};\,\,$ local sections where μ > μCRIT tend to lie close to prestellar cores. (iv) The ability of ppmap to distinguish different types of dust, i.e. dust characterized by different values of the emissivity index, β, reveals that the dust in the filament has a lower emissivity index, β ≲ 1.5, than the dust outside the filament, β ≳ 1.7, implying that the physical conditions in the filament have effected a change in the properties of the dust.

scholarly journals Populations of Hydrogen-like Atoms or Ions and Radio Recombination Lines (RRL's) Interpretation

2002 ◽  
Vol 199 ◽  
pp. 351-352
Author(s):  
N.I. Rovenskaya
Keyword(s):  
Thermal Radiation ◽  
Electron Density ◽  
Hii Regions ◽  
Kinetic Temperature ◽  
Line Radiation ◽  
Continuum Radiation ◽  
Radio Recombination Lines ◽  
The Continuum

The problem of non-LTE populations has been considered in terms of the departure coefficients ∂bn/∂n as functions of the kinetic temperature Te, the electron density Ne, the continuum radiation flow Ic and the ratios of IHnα, IHnβ, IHnδ and IHnε (the line radiation flows). The ratio of IHnα/IHnβ are sensitive to the thermal radiation from HII regions. Characterized by the relation of ∂2bn/∂n2 > 0, the populations are shown to be inhabited radiatively.

scholarly journals 35. Optical emission from the Crab nebula in the continuous spectrum

1957 ◽  
Vol 4 ◽  
pp. 201-204
Author(s):  
I. S. Shklovsky
Keyword(s):  
Thermal Radiation ◽  
Continuous Spectrum ◽  
Crab Nebula ◽  
Optical Emission ◽  
Kinetic Temperature ◽  
Continuous Emission ◽  
The Crab Nebula

All conclusions concerning the nature of the Crab nebula up to the present have been based upon the interpretation of its continuous spectrum given by Baade and Minkowski in their well-known studies ([1, 2]; see also [3, 4]), It was suggested that its continuous emission is a thermal radiation caused by the extremely hot amorphous mass of this nebula. A consequence of this interpretation is that the mass of the envelope is of the order of 10–20 solar masses and the kinetic temperature is extremely high. The filamentary part of the nebula possesses more or less ordinary characteristics.

Sign in / Sign up

Export Citation Format

Share Document