Lyman Alpha Forest
... spectrum there is a relative lack of absorption systems close to the redshift of the QSO. This so-called ‘proximity effect’ has been ascribed to the ionizing radiation produced by the QSO itself, which reduces the neutral hydrogen fraction for gas close to the QSO. The effect can be used to measure ...
... spectrum there is a relative lack of absorption systems close to the redshift of the QSO. This so-called ‘proximity effect’ has been ascribed to the ionizing radiation produced by the QSO itself, which reduces the neutral hydrogen fraction for gas close to the QSO. The effect can be used to measure ...
Molecules Detected in Interstellar Space
... into ‘‘observability’’. As a consequence, the vast majority of interstellar molecules was and still is found in Sgr B2, many of the most complex ones only there. All of the molecules listed in Table 2.1 are found in this source. ...
... into ‘‘observability’’. As a consequence, the vast majority of interstellar molecules was and still is found in Sgr B2, many of the most complex ones only there. All of the molecules listed in Table 2.1 are found in this source. ...
Chap10-Formation
... weigth (~2 mH for gas dominated by H2), T~10 K the gas temperature and ρ the density. The corresponding Jeans Mass is For λ >λJ, thermal pressure cannot resist self-gravity, and runaway collapse follows. ...
... weigth (~2 mH for gas dominated by H2), T~10 K the gas temperature and ρ the density. The corresponding Jeans Mass is For λ >λJ, thermal pressure cannot resist self-gravity, and runaway collapse follows. ...
- UCL Discovery
... smaller C∗ value and lower star formation threshold density (see also Appendix A). We think that this is a part of the reason why high-density threshold of star formation leads to a resultant SFR independent of the parameter C∗ (Saitoh et al. 2008; Hopkins et al. 2013).2 We prefer C∗ = 1 and high nH ...
... smaller C∗ value and lower star formation threshold density (see also Appendix A). We think that this is a part of the reason why high-density threshold of star formation leads to a resultant SFR independent of the parameter C∗ (Saitoh et al. 2008; Hopkins et al. 2013).2 We prefer C∗ = 1 and high nH ...
Feedback from winds and supernovae in massive stellar clusters – I
... been considered by Tan & McKee (2001) and more recently by Harper-Clark & Murray (2009). The latter postulate that the nonuniform surrounding medium causes gaps in the swept-up shell surrounding the wind-blown bubble where some of the high-pressure gas in the bubble interior can leak out. This scena ...
... been considered by Tan & McKee (2001) and more recently by Harper-Clark & Murray (2009). The latter postulate that the nonuniform surrounding medium causes gaps in the swept-up shell surrounding the wind-blown bubble where some of the high-pressure gas in the bubble interior can leak out. This scena ...
Thermal conduction in cosmological SPH simulations
... Thermal conduction in the intracluster medium has been proposed as a possible heating mechanism for offsetting central cooling losses in rich clusters of galaxies. However, because of the coupled non-linear dynamics of gas subject to radiative cooling and thermal conduction, cosmological hydrodynami ...
... Thermal conduction in the intracluster medium has been proposed as a possible heating mechanism for offsetting central cooling losses in rich clusters of galaxies. However, because of the coupled non-linear dynamics of gas subject to radiative cooling and thermal conduction, cosmological hydrodynami ...
The Interstellar Medium in High Redshift Galaxies Comes of Age
... Studying the astrochemistry of the early Universe is crucial for understanding the properties of molecular gas in galaxy formation and for providing fundamental constraints on galaxy evolution. To date, a fairly small number of species, other than CO, have been detected at z > 2 (e.g. HCN, HNC, CN, ...
... Studying the astrochemistry of the early Universe is crucial for understanding the properties of molecular gas in galaxy formation and for providing fundamental constraints on galaxy evolution. To date, a fairly small number of species, other than CO, have been detected at z > 2 (e.g. HCN, HNC, CN, ...
Astrophysics in a Nutshell, Second Edition
... Be can be established, and capture of another 4 He nucleus then completes the triplealpha process. The last stage would have an extremely low probability, were it not for the existence of an excited nuclear energy level in 12 C, which, when added to the rest mass energy of 12 C, happens to have almo ...
... Be can be established, and capture of another 4 He nucleus then completes the triplealpha process. The last stage would have an extremely low probability, were it not for the existence of an excited nuclear energy level in 12 C, which, when added to the rest mass energy of 12 C, happens to have almo ...
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.