The Pluto “Smackdown” and The “New” Solar System
... Differences in organic chemistry important as a function of stellar ...
... Differences in organic chemistry important as a function of stellar ...
Stellar Metamorphosis
... centralizes the majority of the material that forms the theorized disk surrounding it, therefore these stars should not be separate, but should have combined into a single larger star. It is suggested to the reader to realize that gravity theory is a failed theory [13] as it is not a force [14] and ...
... centralizes the majority of the material that forms the theorized disk surrounding it, therefore these stars should not be separate, but should have combined into a single larger star. It is suggested to the reader to realize that gravity theory is a failed theory [13] as it is not a force [14] and ...
First direct mass measurements on nobelium and lawrencium with
... rather limited. Since the binding energy is the reason for the stability of the superheavy elements it is important to have reliable mass values of nuclei in this region. Until 2008 there was no nuclide heavier than uranium whose mass has been measured directly. The masses in this region were based ...
... rather limited. Since the binding energy is the reason for the stability of the superheavy elements it is important to have reliable mass values of nuclei in this region. Until 2008 there was no nuclide heavier than uranium whose mass has been measured directly. The masses in this region were based ...
![arXiv:1102.4757v1 [astro-ph.SR] 23 Feb 2011](http://s1.studyres.com/store/data/017735077_1-cb16692362fed9e2a0fe2690d128f0ce-300x300.png)
arXiv:1102.4757v1 [astro-ph.SR] 23 Feb 2011
... al. 2003). Results for nine binaries discovered in the SPY survey were presented in papers I-V (Napiwotzki et al. 2001, 2002; Karl et al. 2003; Nelemans et al. 2005; Geier et al. 2010a). Subluminous B stars, which are also known as hot sudwarf stars, display the same spectral characteristics as main ...
... al. 2003). Results for nine binaries discovered in the SPY survey were presented in papers I-V (Napiwotzki et al. 2001, 2002; Karl et al. 2003; Nelemans et al. 2005; Geier et al. 2010a). Subluminous B stars, which are also known as hot sudwarf stars, display the same spectral characteristics as main ...
- UCL Discovery
... cluster, which corresponds to 6100 M for the simulation in this paper, where the particle mass is mp = 100 M . Depending on their ID and age, a star particle becomes a feedback particle for some period as described below and then becomes a normal gas particle. In other words, mass-loss from stars ...
... cluster, which corresponds to 6100 M for the simulation in this paper, where the particle mass is mp = 100 M . Depending on their ID and age, a star particle becomes a feedback particle for some period as described below and then becomes a normal gas particle. In other words, mass-loss from stars ...
xrayecc
... star. In larger mass systems, a second mechanism tends to dominate. This is wind driven transfer. Giant stars can lose material from their outer layers, which forms a wind. The companion moves through this wind, and so will accrete matter as it orbits. In this case, the shape of the orbit is importa ...
... star. In larger mass systems, a second mechanism tends to dominate. This is wind driven transfer. Giant stars can lose material from their outer layers, which forms a wind. The companion moves through this wind, and so will accrete matter as it orbits. In this case, the shape of the orbit is importa ...
Evolution of stars
... Protostars are difficult to observe because a. the protostar stage is very short. b. they are surrounded by cocoons of gas and dust. c. they radiate mainly in the infrared. d. all of the above e. they are all so far away that the light hasn't reached us yet. The nuclear reactions in a star's core re ...
... Protostars are difficult to observe because a. the protostar stage is very short. b. they are surrounded by cocoons of gas and dust. c. they radiate mainly in the infrared. d. all of the above e. they are all so far away that the light hasn't reached us yet. The nuclear reactions in a star's core re ...
Star formation and the interstellar medium in galaxy
... the heat input for the gas), collapse time for molecular clouds, and star formation efficiency. In the simulations the star formation quickly settles a kind of thermal equilibrium of the ISM. This result strongly favours the self-regulating mechanism for star formation. The model yields a Schmidt la ...
... the heat input for the gas), collapse time for molecular clouds, and star formation efficiency. In the simulations the star formation quickly settles a kind of thermal equilibrium of the ISM. This result strongly favours the self-regulating mechanism for star formation. The model yields a Schmidt la ...
The star-forming environment of an ultraluminous X-ray
... a small group of OB stars, but is not associated with any massive young clusters nor with any extraordinary massive stars. The brightest point source in the Chandra error circle is consistent with a single blue supergiant (BSG) of mass ≈20 M and age ≈10 Myr. A few other stars are resolved inside th ...
... a small group of OB stars, but is not associated with any massive young clusters nor with any extraordinary massive stars. The brightest point source in the Chandra error circle is consistent with a single blue supergiant (BSG) of mass ≈20 M and age ≈10 Myr. A few other stars are resolved inside th ...
NGC 3801 caught in the act: A post-merger starforming early
... gas outflow or shock heating to have quenched the star formation process in any galaxy is still missing. If in a sample of post-merger ETGs, star formation is found to be on the decline, mass outflow rate is larger than the ongoing star formation rate and AGN feedback timescale coincide with any sha ...
... gas outflow or shock heating to have quenched the star formation process in any galaxy is still missing. If in a sample of post-merger ETGs, star formation is found to be on the decline, mass outflow rate is larger than the ongoing star formation rate and AGN feedback timescale coincide with any sha ...
The star formation history of galaxies in 3D: CALIFA perspective
... 2.1. Hubble sequence: stellar population properties of galaxies in the tuning-fork diagram One step to understand how galaxies form and evolve is classifying galaxies and studying their properties. Most of the massive galaxies in the near Universe are E, S0 and spirals (Blanton & Moustakas 2009), fo ...
... 2.1. Hubble sequence: stellar population properties of galaxies in the tuning-fork diagram One step to understand how galaxies form and evolve is classifying galaxies and studying their properties. Most of the massive galaxies in the near Universe are E, S0 and spirals (Blanton & Moustakas 2009), fo ...
Properties of rapidly rotating PNS with antikaon condensates at
... have been observed in our galaxy[12], many of them can have a period of as low as a millisecond, or a frequency that is greater than 500 Hz. The fastest known pulsar, PSR J1748-2446ad, that has been observed to date was discovered [13] in 2004. It has a rotation period of 1.397 ms and frequency of 7 ...
... have been observed in our galaxy[12], many of them can have a period of as low as a millisecond, or a frequency that is greater than 500 Hz. The fastest known pulsar, PSR J1748-2446ad, that has been observed to date was discovered [13] in 2004. It has a rotation period of 1.397 ms and frequency of 7 ...
Star formation bursts in isolated spiral galaxies
... are rather modest (less than 50 per cent). If, however, the critical density exceeds the mean density by a larger factor, the resulting star formation variations become much more pronounced, as bursts of star formation are associated only with epochs when the form of the spiral pattern in the gas re ...
... are rather modest (less than 50 per cent). If, however, the critical density exceeds the mean density by a larger factor, the resulting star formation variations become much more pronounced, as bursts of star formation are associated only with epochs when the form of the spiral pattern in the gas re ...
6. Stellar Spectra
... Nr,s/N of the lower level of the lines indicated in the upper panel against temperature T (given in units of 1000 K along the top). The pressure was taken constant at Pe = Ne k T = 131 dyne cm-2. The T-axis is adjusted to the abscissa of the upper diagram in order to obtain a correspondence between ...
... Nr,s/N of the lower level of the lines indicated in the upper panel against temperature T (given in units of 1000 K along the top). The pressure was taken constant at Pe = Ne k T = 131 dyne cm-2. The T-axis is adjusted to the abscissa of the upper diagram in order to obtain a correspondence between ...
Measurement of decay time of liquid scintillator
... The decay time constants of LS and GdLS are measured by the start–stop timing method coupled with single photon detection [3]. The system setup is shown in Fig. 1. In this method, the start signal is derived from the plastic scintillator (PS) which is coupled well to an XP2020 photomultiplier tube ( ...
... The decay time constants of LS and GdLS are measured by the start–stop timing method coupled with single photon detection [3]. The system setup is shown in Fig. 1. In this method, the start signal is derived from the plastic scintillator (PS) which is coupled well to an XP2020 photomultiplier tube ( ...
Observations with Herschel: High-mass star formation and the
... is essential to our understanding of the cosmos. When the Earth’s opaque atmosphere prevents the far-infrared radiation to reach ground based antennas, space observatories become crucial to collect that important piece of the large puzzle that otherwise would have been lost. In this thesis, we use o ...
... is essential to our understanding of the cosmos. When the Earth’s opaque atmosphere prevents the far-infrared radiation to reach ground based antennas, space observatories become crucial to collect that important piece of the large puzzle that otherwise would have been lost. In this thesis, we use o ...
PDF hosted at the Radboud Repository of the Radboud University
... (α) is high. Assuming that the efficiency is a universal parameter, this means that the much closer HW Vir binaries should have formed from more massive sdB progenitors and thus should have lower masses (see Hu et al. 2007, Fig. 3) than EGB 5. In contrast, the masses of most sdB primaries in HW Vir sy ...
... (α) is high. Assuming that the efficiency is a universal parameter, this means that the much closer HW Vir binaries should have formed from more massive sdB progenitors and thus should have lower masses (see Hu et al. 2007, Fig. 3) than EGB 5. In contrast, the masses of most sdB primaries in HW Vir sy ...
The chemical case for no winds in dwarf irregular galaxies
... gas-rich dwarf galaxies, not affected by external environmental processes. One of the agents that may regulate the star formation history of these objects is the presence of strong galactic winds. If they have a low mass and a high star formation rate (SFR), the energy injected by supernova (SN) exp ...
... gas-rich dwarf galaxies, not affected by external environmental processes. One of the agents that may regulate the star formation history of these objects is the presence of strong galactic winds. If they have a low mass and a high star formation rate (SFR), the energy injected by supernova (SN) exp ...
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.