1Lec_1 - The University of Texas at Dallas
... two 4-hour courses, each of which has a laboratory component, for a total of 8 semester credit hours of lecture plus laboratory. At UTD, the Biology Department offers two 3-hour lecture courses, Introduction to Modern Biology I and II (BIO 2311, 2312), with associated 1-hour workshops (BIO 2111, 211 ...
... two 4-hour courses, each of which has a laboratory component, for a total of 8 semester credit hours of lecture plus laboratory. At UTD, the Biology Department offers two 3-hour lecture courses, Introduction to Modern Biology I and II (BIO 2311, 2312), with associated 1-hour workshops (BIO 2111, 211 ...
Considerations on the use of atmospheric pressure plasma to generate complex molecular environments with relevance for molecular astrophysics
... carbon and silicon based grains. Biogenic elements (i.e. O, C and N) abundance is around 0.1%, while H and He represents more than 99% of atomic matter [1]. Young stellar objects can be detected within giant molecular clouds and some of these objects are represented by ambient gas at average tempera ...
... carbon and silicon based grains. Biogenic elements (i.e. O, C and N) abundance is around 0.1%, while H and He represents more than 99% of atomic matter [1]. Young stellar objects can be detected within giant molecular clouds and some of these objects are represented by ambient gas at average tempera ...
Massive close binaries, observational characteristics - UvA-DARE
... phase in the evolution of massive close binaries, the formation of LMXBs is an extremely rare event that requires very special initial conditions. This follows immediately from the fact that these systems are very long-lived: their mass transfer phase lasts ~>108 yrs, while there are only some 102 s ...
... phase in the evolution of massive close binaries, the formation of LMXBs is an extremely rare event that requires very special initial conditions. This follows immediately from the fact that these systems are very long-lived: their mass transfer phase lasts ~>108 yrs, while there are only some 102 s ...
Particles and Fundamental Interactions: Supplements, Problems
... logics and triggers of the experimental apparatuses, ending with the computing effort required for the LHC collider. These issues play also a key role in the contribution that particle physics research provides as a spin-off technology. This is also true for other four supplements, presenting additi ...
... logics and triggers of the experimental apparatuses, ending with the computing effort required for the LHC collider. These issues play also a key role in the contribution that particle physics research provides as a spin-off technology. This is also true for other four supplements, presenting additi ...
PoS(ICRC2015)509
... It is well known that particle acceleration occurs in environments where a collisionless plasma forms a shock front, resulting in a power law energy spectrum of the non-thermal population (e.g. [1, 2] and references therein). Due to their features, Colliding Wind Binaries (CWBs) are expected to be s ...
... It is well known that particle acceleration occurs in environments where a collisionless plasma forms a shock front, resulting in a power law energy spectrum of the non-thermal population (e.g. [1, 2] and references therein). Due to their features, Colliding Wind Binaries (CWBs) are expected to be s ...
Fundamentals of NMR
... This two-state description is appropriate for most nuclei of biologic interest including 1H, 13C, 15N, 19F, and 31P; i.e., all those which have nuclear spin quantum number I = l/2. It is a quantum mechanical requirement that any individual nuclear spins of a nucleus with I = l/2 be in one of the tw ...
... This two-state description is appropriate for most nuclei of biologic interest including 1H, 13C, 15N, 19F, and 31P; i.e., all those which have nuclear spin quantum number I = l/2. It is a quantum mechanical requirement that any individual nuclear spins of a nucleus with I = l/2 be in one of the tw ...
Chapter 1 Fundamentals of NMR
... This two-state description is appropriate for most nuclei of biologic interest including 1H, 13C, 15N, 19F, and 31P; i.e., all those which have nuclear spin quantum number I = l/2. It is a quantum mechanical requirement that any individual nuclear spins of a nucleus with I = l/2 be in one of the tw ...
... This two-state description is appropriate for most nuclei of biologic interest including 1H, 13C, 15N, 19F, and 31P; i.e., all those which have nuclear spin quantum number I = l/2. It is a quantum mechanical requirement that any individual nuclear spins of a nucleus with I = l/2 be in one of the tw ...
Sub-luminous type Ia supernovae from the mergers of equal
... mergers with mass ratios close to one, systems with total mass similar to that in our simulation are the most relevant case for SNe Ia. Although lower-mass systems will be more common, they will not lead to a detonation as discussed above. Thus they will not result in SNe Ia, but may be observable a ...
... mergers with mass ratios close to one, systems with total mass similar to that in our simulation are the most relevant case for SNe Ia. Although lower-mass systems will be more common, they will not lead to a detonation as discussed above. Thus they will not result in SNe Ia, but may be observable a ...
Multiphoton interactions in lepton photoproduction on nuclei at high
... plitude illZ through the dipole-proton one illp . This can be done if the nuclear protons can be considered as independent scattering centers. For large Z their distribution thus follows the Poisson law that leads to a particularly simple expression for the amplitude (10). To avoid possible confus ...
... plitude illZ through the dipole-proton one illp . This can be done if the nuclear protons can be considered as independent scattering centers. For large Z their distribution thus follows the Poisson law that leads to a particularly simple expression for the amplitude (10). To avoid possible confus ...
The Most Massive LMC Star Sk
... stars, as the formation of low mass stars from the IUE data concluded that R 136 a is a single supermassive star of needs a longer time scale. This may be a general trend of massive star formation - 3,000 MG emitting an extremely powerful wind of 10-3 ,5 MG yr- 1 at 3,500 that they form in groups. T ...
... stars, as the formation of low mass stars from the IUE data concluded that R 136 a is a single supermassive star of needs a longer time scale. This may be a general trend of massive star formation - 3,000 MG emitting an extremely powerful wind of 10-3 ,5 MG yr- 1 at 3,500 that they form in groups. T ...
Surface tension of compressed, superheavy atoms
... atom composed by a superheavy nuclear core (superheavy nucleus), and degenerate electrons that neutralize the system. Some electrons penetrate into the superheavy nuclear core and the rest surround it up to a distance that depends upon the compression level. Such kind of compressed, superheavy atoms ...
... atom composed by a superheavy nuclear core (superheavy nucleus), and degenerate electrons that neutralize the system. Some electrons penetrate into the superheavy nuclear core and the rest surround it up to a distance that depends upon the compression level. Such kind of compressed, superheavy atoms ...
Introducing the fission–fusion reaction process: using a
... the r-process is slowed down due to low neutron-capture cross sections when going beyond the magic neutron numbers. These decisive bottlenecks of the r-process flow are called waiting points [10]. The astrophysical site of the r-process nucleosynthesis is still under debate: it may be cataclysmic co ...
... the r-process is slowed down due to low neutron-capture cross sections when going beyond the magic neutron numbers. These decisive bottlenecks of the r-process flow are called waiting points [10]. The astrophysical site of the r-process nucleosynthesis is still under debate: it may be cataclysmic co ...
Here`s
... do not see the unique gamma rays that are produced when antimatter annihilates with matter. Finally, we can rule out large galaxy-sized black holes on the basis of how many gravitational lenses we see. High concentrations of matter bend light passing near them from objects further away, but we do no ...
... do not see the unique gamma rays that are produced when antimatter annihilates with matter. Finally, we can rule out large galaxy-sized black holes on the basis of how many gravitational lenses we see. High concentrations of matter bend light passing near them from objects further away, but we do no ...
Stardust--Snapshots of Stars
... stars. However, some of the grains found in the study do not fit within this framework, and require different astrophysical origins. One grain has massive enrichments in 17O, 25Mg, and 26Mg, which are considered isotopic signatures of condensation from nova ejecta. Two other spinel grains have large ...
... stars. However, some of the grains found in the study do not fit within this framework, and require different astrophysical origins. One grain has massive enrichments in 17O, 25Mg, and 26Mg, which are considered isotopic signatures of condensation from nova ejecta. Two other spinel grains have large ...
1 The Physical Basis of NMR Spectroscopy
... Therefore the only transitions that can take place are those between adjacent energy levels. According to this selection rule the transition from m = + 1 to m = _ 1 for a 14N nucleus is forbidden. Although coupled spin systems will not be treated until later, we shall point out here that a simultane ...
... Therefore the only transitions that can take place are those between adjacent energy levels. According to this selection rule the transition from m = + 1 to m = _ 1 for a 14N nucleus is forbidden. Although coupled spin systems will not be treated until later, we shall point out here that a simultane ...
Introduction to the Monte Carlo Method
... 1 I’m positive I’m proton!! very important. It changes what we 2 Yes, I am energetic enough to pass the threshold!! understand by moving in a simulation. 3 ComputeIn total meanmoving free path λ and general, is not justdistance a changeto boundary (sgeo ), sample step sλbut anda get maximum allowed ...
... 1 I’m positive I’m proton!! very important. It changes what we 2 Yes, I am energetic enough to pass the threshold!! understand by moving in a simulation. 3 ComputeIn total meanmoving free path λ and general, is not justdistance a changeto boundary (sgeo ), sample step sλbut anda get maximum allowed ...
P-nuclei
p-Nuclei (p stands for proton-rich) are certain proton-rich, naturally occurring isotopes of some elements between selenium and mercury which cannot be produced in either s- or r-process.