Models of the Structure and Evolution of Protoplanetary Disks
... In reality protoplanetary disks are not quite steady. After the main infall phase is over, the disk is not supplied anymore with new matter, and the continuing accretion onto the star will drain matter from the disk (see Fig. 1). In addition the disk viscously expands and is subject to photoevaporat ...
... In reality protoplanetary disks are not quite steady. After the main infall phase is over, the disk is not supplied anymore with new matter, and the continuing accretion onto the star will drain matter from the disk (see Fig. 1). In addition the disk viscously expands and is subject to photoevaporat ...
Ch a n d
... various kinds of mass outflow. The impact of plasma onto the stellar surface from magnetospheric accretion streams, can be a dominant source of energy and momentum in the upper atmospheres of T Tauri stars. We present models in which turbulence is induced by these impacts, and waves then spread out ...
... various kinds of mass outflow. The impact of plasma onto the stellar surface from magnetospheric accretion streams, can be a dominant source of energy and momentum in the upper atmospheres of T Tauri stars. We present models in which turbulence is induced by these impacts, and waves then spread out ...
Doeleman_Haystack_Requirements_Astronomy
... • Lens theory predicts ‘odd’ number of images, but almost all systems have 2 or 4: a mystery. B2114+022 ...
... • Lens theory predicts ‘odd’ number of images, but almost all systems have 2 or 4: a mystery. B2114+022 ...
Liverpool Telescope 2: a new robotic facility for rapid transient follow
... Despite their importance, we still know embarrassingly little about SNe Ia. The nature of the progenitor system is hotly debated, spurred by searches for surviving companions (Ruiz-Lapuente et al, 2004), traces of hydrogen from the companion (Mattila et al, 2005), or bumps in the light curves caused ...
... Despite their importance, we still know embarrassingly little about SNe Ia. The nature of the progenitor system is hotly debated, spurred by searches for surviving companions (Ruiz-Lapuente et al, 2004), traces of hydrogen from the companion (Mattila et al, 2005), or bumps in the light curves caused ...
Abstract Title of Dissertation: BLACK HOLE DYNAMICS AND GRAVITATIONAL RADIATION IN GALACTIC NUCLEI
... that host supermassive black holes. Mergers between stellar-mass black holes will be key sources of gravitational radiation for ground-based detectors. However, the rates of these events are highly uncertain, because we can not observe these binaries electromagnetically. In this work, we show that t ...
... that host supermassive black holes. Mergers between stellar-mass black holes will be key sources of gravitational radiation for ground-based detectors. However, the rates of these events are highly uncertain, because we can not observe these binaries electromagnetically. In this work, we show that t ...
The galaxy stellar mass function at 3.5 ≤z ≤ 7.5 in the CANDELS
... Context. The form and evolution of the galaxy stellar mass function (GSMF) at high redshifts provide crucial information on star formation history and mass assembly in the young Universe, close or even prior to the epoch of reionization. Aims. We used the unique combination of deep optical/near-infr ...
... Context. The form and evolution of the galaxy stellar mass function (GSMF) at high redshifts provide crucial information on star formation history and mass assembly in the young Universe, close or even prior to the epoch of reionization. Aims. We used the unique combination of deep optical/near-infr ...
Three Binary Millisecond Pulsars in NGC 6266
... for pulsars in the system of southern GCs using the Parkes 64 m radio telescope that commenced in 2000. It exploits the high sensitivity of the central beam of the Parkes multibeam receiver (Staveley-Smith et al. 1996), the efficiency of a modern data acquisition system (e.g., Manchester et al. 2001; ...
... for pulsars in the system of southern GCs using the Parkes 64 m radio telescope that commenced in 2000. It exploits the high sensitivity of the central beam of the Parkes multibeam receiver (Staveley-Smith et al. 1996), the efficiency of a modern data acquisition system (e.g., Manchester et al. 2001; ...
betelgeuse and the red supergiants
... Betelgeuse’s fate depends to a large degree on its birth mass. If sufficiently massive, it will end as a core-collapse supernova leaving a neutron star or black hole. But do we know that it is? If Betelgeuse were to be a lower-mass super-Asymptotic Giant Branch (super-AGB) star it would end up as an ...
... Betelgeuse’s fate depends to a large degree on its birth mass. If sufficiently massive, it will end as a core-collapse supernova leaving a neutron star or black hole. But do we know that it is? If Betelgeuse were to be a lower-mass super-Asymptotic Giant Branch (super-AGB) star it would end up as an ...
Applications of Photospheric Spot Temperature Models ... Stellar Angular Momentum Evolution
... We apply a simple photospheric spot temperature model to photometric variability measurements of T Tauri stars in the Trapezium region of the Orion Nebula Cluster. Our aim is to search for the relationship , if any, between spot temperatures and stellar rotation periods to better understand the rela ...
... We apply a simple photospheric spot temperature model to photometric variability measurements of T Tauri stars in the Trapezium region of the Orion Nebula Cluster. Our aim is to search for the relationship , if any, between spot temperatures and stellar rotation periods to better understand the rela ...
Coded Aperture Imaging of Nuclear Fusion In The Plasma Focus
... experiments, two larger coded masks: mask-1345 (91×15 array and 341 holes each 0.3 mm side) and mask-4680 (104×45 arrays and 585 holes each 0.27 mm side) were placed at 90° to the plasma focus axis to investigate the fusion source in pure deuterium and deuterium-krypton admixture working gases. The ...
... experiments, two larger coded masks: mask-1345 (91×15 array and 341 holes each 0.3 mm side) and mask-4680 (104×45 arrays and 585 holes each 0.27 mm side) were placed at 90° to the plasma focus axis to investigate the fusion source in pure deuterium and deuterium-krypton admixture working gases. The ...
Heating and cooling of accreting white dwarfs
... forms an accretion disc around the white dwarf, spiralling slowly inwards while transforming kinetic energy into heat by viscous friction. In this case, the white dwarf will accrete from the inner disc through an equatorial belt. Both types of systems, however, share a common fate: once a certain am ...
... forms an accretion disc around the white dwarf, spiralling slowly inwards while transforming kinetic energy into heat by viscous friction. In this case, the white dwarf will accrete from the inner disc through an equatorial belt. Both types of systems, however, share a common fate: once a certain am ...
doctoral thesis (Dissertation)
... and UV spectroscopy and through detailed physical simulations. Spectroscopic X-ray data is reduced and presented for two targets: The CTTS V4046 Sgr was observed with Chandra for 100 ks, using a high-resolution grating spectrometer. The lightcurve contains one flare and the He-like triplets of Si xi ...
... and UV spectroscopy and through detailed physical simulations. Spectroscopic X-ray data is reduced and presented for two targets: The CTTS V4046 Sgr was observed with Chandra for 100 ks, using a high-resolution grating spectrometer. The lightcurve contains one flare and the He-like triplets of Si xi ...
A Theory of Extrasolar Giant Planets
... but which dier in detail from solar composition in that they are enhanced in metals by about one order of magnitude, with a substantial quantity of these heavier elements concentrated toward their centers. The purpose of this paper is to provide accurate and extensive models of extrasolar giant pla ...
... but which dier in detail from solar composition in that they are enhanced in metals by about one order of magnitude, with a substantial quantity of these heavier elements concentrated toward their centers. The purpose of this paper is to provide accurate and extensive models of extrasolar giant pla ...
Star formation in luminous quasar host galaxies at z = 1–2 ⋆
... A key observable is the level of star formation present in quasar host galaxies when compared to inactive galaxies of the same mass at the same epoch. In this paper, we aim to explore the level of star formation in our z ≈ 1 and 2 quasar samples, originally imaged in the rest-frame optical using HST ...
... A key observable is the level of star formation present in quasar host galaxies when compared to inactive galaxies of the same mass at the same epoch. In this paper, we aim to explore the level of star formation in our z ≈ 1 and 2 quasar samples, originally imaged in the rest-frame optical using HST ...
Stellar activity in exoplanet hosts Enrique Herrero Casas
... stars for a targeted transit search was presented. A search within this subset would have an expected rate of findings increased in a factor of 2 o 3 with respect to a search on the initial sample (Herrero et al. 2012). The high precision photometry provided by the space missions Kepler and CoRoT has ...
... stars for a targeted transit search was presented. A search within this subset would have an expected rate of findings increased in a factor of 2 o 3 with respect to a search on the initial sample (Herrero et al. 2012). The high precision photometry provided by the space missions Kepler and CoRoT has ...
Coherent Control of Polarized Neutron Interferometry
... interferometer to separate two paths where spin states are independently manipulated. The final measurement is made on the spin degree of freedom, so we observe spinbased contrast without a need for coherence in the path degree of freedom. This is difficult to achieve in a spin-echo interferometer b ...
... interferometer to separate two paths where spin states are independently manipulated. The final measurement is made on the spin degree of freedom, so we observe spinbased contrast without a need for coherence in the path degree of freedom. This is difficult to achieve in a spin-echo interferometer b ...
THE NEW GALAXY: Signatures of Its Formation
... to a disk for the first time. Two key observations emphasize what we consider to be the mystery of the main epoch of baryon dissipation. First, there are no stars with [Fe/H] < −2.2 that rotate with the disk. Second, despite all the activity associated with the Golden Age, at least 80% of the baryon ...
... to a disk for the first time. Two key observations emphasize what we consider to be the mystery of the main epoch of baryon dissipation. First, there are no stars with [Fe/H] < −2.2 that rotate with the disk. Second, despite all the activity associated with the Golden Age, at least 80% of the baryon ...
Decoding Galaxy Evolution with Gas
... long-lived asymptotic giant branch stars that is absent from the bulge PC2 because of rapid bulge formation. Detailed interpretations of stellar abundance patterns require chemical evolution modeling, but these models are sensitive to the treatment of star formation efficiency (SFE), outflow, stellar y ...
... long-lived asymptotic giant branch stars that is absent from the bulge PC2 because of rapid bulge formation. Detailed interpretations of stellar abundance patterns require chemical evolution modeling, but these models are sensitive to the treatment of star formation efficiency (SFE), outflow, stellar y ...
Population synthesis for double white dwarfs. I. Close - UvA-DARE
... Much less frequently, CO white dwarfs are formed by stars more massive than 2.3 M which fill their Roche lobe when they have a nondegenerate core, before helium ignition. Roche lobe overflow then results in the formation of a low-mass helium star. A brief additional phase of mass transfer may happe ...
... Much less frequently, CO white dwarfs are formed by stars more massive than 2.3 M which fill their Roche lobe when they have a nondegenerate core, before helium ignition. Roche lobe overflow then results in the formation of a low-mass helium star. A brief additional phase of mass transfer may happe ...
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.