Radial transport in the solar nebula: Implications for moderately
... which determined the rates of mass and angular momentum transport. This was done to avoid having to define a process that would be responsible for driving mass transport in protoplanetary disk. This driving force remains the subject of ongoing research today. As such, the use of the α-viscosity does ...
... which determined the rates of mass and angular momentum transport. This was done to avoid having to define a process that would be responsible for driving mass transport in protoplanetary disk. This driving force remains the subject of ongoing research today. As such, the use of the α-viscosity does ...
Massive quiescent galaxies at cosmic noon Robert Feldmann UC Berkeley
... Fig. 2.— Upper : ALMA 870µm continuum map of SGP38326. The three detected SMGs are indicated. The grey contours represent the integrated 12 CO(5–4) emission. This line is clearly detected in both SMG1 and SMG2, but there is no 12 CO(5–4) detection in SMG3. The beam sizes of the 12 CO(5–4) (grey elli ...
... Fig. 2.— Upper : ALMA 870µm continuum map of SGP38326. The three detected SMGs are indicated. The grey contours represent the integrated 12 CO(5–4) emission. This line is clearly detected in both SMG1 and SMG2, but there is no 12 CO(5–4) detection in SMG3. The beam sizes of the 12 CO(5–4) (grey elli ...
The Kuiper Belt: What We Know and What We Don`t - UCLA
... on the assumption that the Kuiper belt was much more massive than it is now (e.g. 30 Earth masses, or about 300 times the present mass). This raises the obvious question: where did all this initial mass go? One suggestion is that the depletion of the Kuiper belt could have been caused by extensive ...
... on the assumption that the Kuiper belt was much more massive than it is now (e.g. 30 Earth masses, or about 300 times the present mass). This raises the obvious question: where did all this initial mass go? One suggestion is that the depletion of the Kuiper belt could have been caused by extensive ...
The role of the initial surface density profiles of the disc on giant
... not have consequences on the formation of the others. Despite this model is a reasonable good approximation in the intermediate region of the solar nebula, posses too much surface density in the inner region, underpredicts it in the outer nebula, and the total mass of the disc is infinite in this fo ...
... not have consequences on the formation of the others. Despite this model is a reasonable good approximation in the intermediate region of the solar nebula, posses too much surface density in the inner region, underpredicts it in the outer nebula, and the total mass of the disc is infinite in this fo ...
Star Formation: Chemistry as a Probe of Embedded Protostars
... spectrally unresolved.1 I will discuss the CO rotational lines in more detail as an example of both the opportunities and the limitations from the Herschel observations. Rotationally excited CO is ubiquitous in low-mass embedded protostars. Early observations with ground-based sub-millimeter telesco ...
... spectrally unresolved.1 I will discuss the CO rotational lines in more detail as an example of both the opportunities and the limitations from the Herschel observations. Rotationally excited CO is ubiquitous in low-mass embedded protostars. Early observations with ground-based sub-millimeter telesco ...
Feedback from winds and supernovae in massive stellar clusters – I
... Rosette nebula reveals that only a small proportion of the cluster wind energy is radiated in the X-ray, and Townsley et al. (2003) conclude that most of the hot gas must flow without cooling into the wider ISM. This picture is supported by the analysis of the Omega nebula, the Arches cluster and NG ...
... Rosette nebula reveals that only a small proportion of the cluster wind energy is radiated in the X-ray, and Townsley et al. (2003) conclude that most of the hot gas must flow without cooling into the wider ISM. This picture is supported by the analysis of the Omega nebula, the Arches cluster and NG ...
Evolution and colors of helium-core white dwarf stars with high
... The study of the evolution of low-mass He white dwarfs has captured the attention of researchers since Kippenhahn et al. (1967) suggested that these stars could be the natural result of substantial mass loss from low-mass red giant stars filling their Roche lobes in binary systems. Later, Webbink (1 ...
... The study of the evolution of low-mass He white dwarfs has captured the attention of researchers since Kippenhahn et al. (1967) suggested that these stars could be the natural result of substantial mass loss from low-mass red giant stars filling their Roche lobes in binary systems. Later, Webbink (1 ...
Maximum Mass Restraint of Neutron Stars
... the core it begins accumulating until it reaches approximately 1.44 solar masses. At this point degeneracy pressures can no longer support the core and the process of star collapse begins. Core collapse is a rather violent process and is caused by the production of gamma rays within the core. Throug ...
... the core it begins accumulating until it reaches approximately 1.44 solar masses. At this point degeneracy pressures can no longer support the core and the process of star collapse begins. Core collapse is a rather violent process and is caused by the production of gamma rays within the core. Throug ...
Physics modules P7 - Higher
... When a large amount of gas in space is compressed a star is formed. As the gas compresses the temperature of the gas increases. As the temperature increases, the pressure in the gas changes. Explain how the pressure changes. Your answer should include ...
... When a large amount of gas in space is compressed a star is formed. As the gas compresses the temperature of the gas increases. As the temperature increases, the pressure in the gas changes. Explain how the pressure changes. Your answer should include ...
PDF only - at www.arxiv.org.
... Our comparison observations consist of 1.0-4.5 µm disk-integrated NIR spectra taken of the Earth by the HRI instrument on the Deep Impact flyby spacecraft (Hampton et al. 2005; Klaasen et al. 2008) as part of the EPOXI mission. We present data model comparisons for four observations taken from 2008- ...
... Our comparison observations consist of 1.0-4.5 µm disk-integrated NIR spectra taken of the Earth by the HRI instrument on the Deep Impact flyby spacecraft (Hampton et al. 2005; Klaasen et al. 2008) as part of the EPOXI mission. We present data model comparisons for four observations taken from 2008- ...
High Resolution Chandra Spectroscopy of Gamma Cassiopeia (B0
... SRH98). Highly redshifted spectral lines in the UV (Smith & Robinson 1999) are indicative of high velocity plasmoids, with energies comparable to the X-ray flux and suggest the interaction of X-ray emitting volumes with a circumstellar structure, probably the dense disk of the Be star. There is indi ...
... SRH98). Highly redshifted spectral lines in the UV (Smith & Robinson 1999) are indicative of high velocity plasmoids, with energies comparable to the X-ray flux and suggest the interaction of X-ray emitting volumes with a circumstellar structure, probably the dense disk of the Be star. There is indi ...
Massive z~1.3 evolved galaxies revealed
... does not make sense since these ages are much larger than the Hubble time at z ∼ 1.2. By forcing galaxies to have ages lower than the Hubble time at this z the only good result is obtained with Z = 2 Z models which provide a good fit to the data in the case of a 3.5 Gyr old τ = 0.1 (P(χ̃2 ) 0.95) ...
... does not make sense since these ages are much larger than the Hubble time at z ∼ 1.2. By forcing galaxies to have ages lower than the Hubble time at this z the only good result is obtained with Z = 2 Z models which provide a good fit to the data in the case of a 3.5 Gyr old τ = 0.1 (P(χ̃2 ) 0.95) ...
Dynamics of the Milky Way
... • Relaxation is expected to have occurred in some globular clusters and the densest nuclei of galaxies Dynamics of the Milky Way --- Part 1: Introduction and Fundamental Stellar Dynamics ...
... • Relaxation is expected to have occurred in some globular clusters and the densest nuclei of galaxies Dynamics of the Milky Way --- Part 1: Introduction and Fundamental Stellar Dynamics ...
The star-forming environment of an ultraluminous X-ray
... two groups of blue and red stars (Fig. 4). The latter (m 555 − m 814 0.7) are easily identified as red supergiants (RSGs; stars with shell hydrogen or, later, shell Helium burning); we find 46 of them. The blue stars comprise blue supergiants (BSGs; stars in their coreHelium-burning phase of evolu ...
... two groups of blue and red stars (Fig. 4). The latter (m 555 − m 814 0.7) are easily identified as red supergiants (RSGs; stars with shell hydrogen or, later, shell Helium burning); we find 46 of them. The blue stars comprise blue supergiants (BSGs; stars in their coreHelium-burning phase of evolu ...
Significance of the Kuiper Belt
... on the assumption that the Kuiper belt was much more massive than it is now (e.g. 30 Earth masses, or about 300 times the present mass). This raises the obvious question: where did all this initial mass go?!! One suggestion is that the depletion of the Kuiper belt could have been caused by extensive ...
... on the assumption that the Kuiper belt was much more massive than it is now (e.g. 30 Earth masses, or about 300 times the present mass). This raises the obvious question: where did all this initial mass go?!! One suggestion is that the depletion of the Kuiper belt could have been caused by extensive ...
NEAR-INFRARED THERMAL EMISSION FROM THE HOT JUPITER
... sky subtraction, zero-point calibration, and a rough astrometry determination. We sky subtract our data by constructing a normalized sky frame built by taking the median of a stack of source-masked and background-normalized on-sky images. Our on-sky images consist of 15 dithered in-focus images obse ...
... sky subtraction, zero-point calibration, and a rough astrometry determination. We sky subtract our data by constructing a normalized sky frame built by taking the median of a stack of source-masked and background-normalized on-sky images. Our on-sky images consist of 15 dithered in-focus images obse ...
The effect of starspots on the radii of low-mass
... would adapt on the Kelvin–Helmholtz time-scale of the convective envelope to achieve thermal equilibrium. For low-mass stars with deep convective envelopes they used a polytropic model to show that the effect of starspots is to reduce the luminosity of the star at near-constant radius and temperatur ...
... would adapt on the Kelvin–Helmholtz time-scale of the convective envelope to achieve thermal equilibrium. For low-mass stars with deep convective envelopes they used a polytropic model to show that the effect of starspots is to reduce the luminosity of the star at near-constant radius and temperatur ...