Complex organic molecules along the accretion flow in isolated and
... low-mass star formation, respectively. One proposed mechanism for forming COMs in these sources is that simple ices formed on grain surfaces at 10 K (e.g., CO, H2 O, NH3 , CH4 , and CH3 OH) undergo warming to ≈ 20 – 30 K (caused by the ignition of the embedded star) where the grain-surface molecule ...
... low-mass star formation, respectively. One proposed mechanism for forming COMs in these sources is that simple ices formed on grain surfaces at 10 K (e.g., CO, H2 O, NH3 , CH4 , and CH3 OH) undergo warming to ≈ 20 – 30 K (caused by the ignition of the embedded star) where the grain-surface molecule ...
molecular dynamics studies of the stability of co2
... pressure conditions were tried before choosing these conditions. The temperature was chosen so that it is within the hydrate stability zone but not too far from the hydrate dissociation point at the chosen pressure, so that considerable amount of dissolution is observed with both methane and CO2 hyd ...
... pressure conditions were tried before choosing these conditions. The temperature was chosen so that it is within the hydrate stability zone but not too far from the hydrate dissociation point at the chosen pressure, so that considerable amount of dissolution is observed with both methane and CO2 hyd ...
Chapter 1
... The optical emission line spectrum contains the Balmer series of Hydrogen (e.g., Hδ, Hγ, Hβ, Hα), together with lines of Helium (e.g., He ii λ4686) and numerous other emission lines such as Oxygen (e.g., [O i] λ6300, [O ii] λ3726, [O iii] λ5007), Nitrogen (e.g., [N ii]λ6584), Sulfur (e.g., [S ii]λ67 ...
... The optical emission line spectrum contains the Balmer series of Hydrogen (e.g., Hδ, Hγ, Hβ, Hα), together with lines of Helium (e.g., He ii λ4686) and numerous other emission lines such as Oxygen (e.g., [O i] λ6300, [O ii] λ3726, [O iii] λ5007), Nitrogen (e.g., [N ii]λ6584), Sulfur (e.g., [S ii]λ67 ...
The Atoms that Vanish
... Let's see what this involves in a particular case. Suppose we and suppose that it take a kind of atom we will call Atom ...
... Let's see what this involves in a particular case. Suppose we and suppose that it take a kind of atom we will call Atom ...
Hot Gas In and Around Elliptical Galaxies William G. Mathews
... flows is often highly disturbed. Evidently, massive black holes, thought to inhabit the cores of all stellar bulges, may become energy sources when stimulated by inflowing hot gas. Can the central heating visible in Chandra images explain the absence of cooling in XMM spectra? This is one of many fu ...
... flows is often highly disturbed. Evidently, massive black holes, thought to inhabit the cores of all stellar bulges, may become energy sources when stimulated by inflowing hot gas. Can the central heating visible in Chandra images explain the absence of cooling in XMM spectra? This is one of many fu ...
Rapid neutral–neutral reactions at low temperatures
... et al. (1994) and Bettens, Lee & Herbst (1995), the latter referring to their network as the ‘new neutral–neutral model (nnnm)’. In these networks, the small number of low-temperature studies then extant was generalized based on the chemical intuition of the authors. In general, the models failed to ...
... et al. (1994) and Bettens, Lee & Herbst (1995), the latter referring to their network as the ‘new neutral–neutral model (nnnm)’. In these networks, the small number of low-temperature studies then extant was generalized based on the chemical intuition of the authors. In general, the models failed to ...
Kinematics of Arp 270: gas flows, nuclear activity
... of them for attenuation, so the values we give are lower limits to the SFR. It is significant that NGC 3395 is more affected by dust attenuation than NGC 3996 as we will comment below. 3 G L O BA L K I N E M AT I C S The velocity map in Fig. 2 shows a distorted rotation field in NGC 3395, and an app ...
... of them for attenuation, so the values we give are lower limits to the SFR. It is significant that NGC 3395 is more affected by dust attenuation than NGC 3996 as we will comment below. 3 G L O BA L K I N E M AT I C S The velocity map in Fig. 2 shows a distorted rotation field in NGC 3395, and an app ...
New SPIS capabilities to simulate dust electrostatic charging
... The latter is expected to be amplified by the lighting variation on the irregular moon surface, in particular close to the crater rims. The ejected dust particles can be deposited on landers on the moon surface. To investigate for potential lunar mission risks, the capabilities of the Spacecraft-Pla ...
... The latter is expected to be amplified by the lighting variation on the irregular moon surface, in particular close to the crater rims. The ejected dust particles can be deposited on landers on the moon surface. To investigate for potential lunar mission risks, the capabilities of the Spacecraft-Pla ...
MOLECULAR CLOUDS 1. Introduction
... formation time equals the dissolution time, then, averaged over the Galaxy, there would have to be approximately equal gas masses in GMCs and in the cha. As Cowie (1980) showed, this need only to be true in the spiral arms, since orbit crowding can enhance the surface density of small clouds in the ...
... formation time equals the dissolution time, then, averaged over the Galaxy, there would have to be approximately equal gas masses in GMCs and in the cha. As Cowie (1980) showed, this need only to be true in the spiral arms, since orbit crowding can enhance the surface density of small clouds in the ...
A Comparison of Modeled and Measured Surface Shortwave
... showed that their model, with the best available gaseous absorption cross section data, accurately computes direct irradiance provided that the model has as input accurate water vapor and ozone profiles and extinction optical thickness of the atmosphere at a set of discrete wavelengths. However, the ...
... showed that their model, with the best available gaseous absorption cross section data, accurately computes direct irradiance provided that the model has as input accurate water vapor and ozone profiles and extinction optical thickness of the atmosphere at a set of discrete wavelengths. However, the ...
Microplasma
Microplasmas are plasmas of small dimensions, ranging from tens to thousands of micrometers. They can be generated at a variety of temperatures and pressures, existing as either thermal or non-thermal plasmas. Non-thermal microplasmas that can maintain their state at standard temperatures and pressures are readily available and accessible to scientists as they can be easily sustained and manipulated under standard conditions. Therefore, they can be employed for commercial, industrial, and medical applications, giving rise to the evolving field of microplasmas.