Sökning: "protoplanetary disk evolution"

Hittade 5 uppsatser innehållade orden protoplanetary disk evolution.

1. 1. The fate of pebbles and planetesimals entering protoplanetary envelopes

   Master-uppsats, Lunds universitet/Astronomi - Genomgår omorganisation

   Författare :Emil Zadera; [2019]
   Nyckelord :Planet formation; planet; protoplanet; protoplanetary envelope; protoplanetary atmosphere; protoplanetary growth; planetary growth model; accretion rate; vapour blob; vapourblob; vapour planet; transport of water; water on planet; pebbles; planetesimals; pebble accretion; planetesimal accretion; meteors; ablation; fragmentation; sublimation; protoplanetary disk; MMSN; accretion window; accretion channel; accretion; destruction; disruption; terminal velocity; gas; gasflow; shearingbox; exoplanet; Physics and Astronomy;

   Sammanfattning : Planetary embryos grow by the accretion of solid dust-material, ranging from cm- to m-sized pebbles up to km-sized planetesimals. However, the underlying size-distribution of the accreted material is poorly understood. LÄS MER

3. 2. Formation and Evolution of Protoplanetary Disks

   Master-uppsats, Lunds universitet/Astronomi - Genomgår omorganisation

   Författare :Johan Appelgren; [2019]
   Nyckelord :protoplanetary disk; protoplanetary disk formation; protoplanetary disk evolution; planet formation; Physics and Astronomy;

   Sammanfattning : A star forms with a surrounding protoplanetary disk after the collapse of a molecular cloud core. Subsequently, over a period of several Myr this protoplanetary disk of dust and gas is accreted onto the host star. We model the formation and evolution of such a protoplanetary disk using a one-dimensional numerical model. LÄS MER

4. 3. Mean Motion Resonances and Planetary Scattering

   Master-uppsats, Lunds universitet/Astronomi - Genomgår omorganisation; Lunds universitet/Institutionen för astronomi och teoretisk fysik - Genomgår omorganisation

   Författare :Erik Dahlöf; [2018]
   Nyckelord :mean motion resonance; orbit resonance; planetary dynamics; planet-planet scattering; planetary scattering; eccentricity; inclination; planet systems; disturbing force; orbit dynamics; orbital elements; planets; exoplanets; scattering phase; relaxation; dynamical instabilities; N-body; protoplanetary disk; planet migration; eccentricity damping; inclination damping; planet-disk interactions; Physics and Astronomy;

   Sammanfattning : The observed distribution of giant exoplanet eccentricities and inclinations are significantly larger than what is measured for their Solar system analogues, Jupiter and Saturn. Since the first observations of exoplanets, planet-planet scattering has been proposed as a possible mechanism for exciting the eccentricities and inclinations of giant exoplanets. LÄS MER

5. 4. Planet migration in evolving protoplanetary discs

   Master-uppsats, Lunds universitet/Astronomi - Genomgår omorganisation; Lunds universitet/Institutionen för astronomi och teoretisk fysik - Genomgår omorganisation

   Författare :Linn Eriksson; [2018]
   Nyckelord :Planets and satellites: formation; Protoplanetary discs: evolution; Planet-disc interactions; Physics and Astronomy;

   Sammanfattning : The rate of migration and accretion onto protoplanets is greatly influenced by the structure of the surrounding protoplanetary disc. This structure changes with time as the disc evolves on a million year timescale, implying that the process of planet formation might look very different depending on when it was initiated. LÄS MER

7. 5. Giant planet formation around HR8799

   Master-uppsats, Lunds universitet/Astronomi - Genomgår omorganisation; Lunds universitet/Institutionen för astronomi och teoretisk fysik - Genomgår omorganisation

   Författare :Dan Wallsby; [2017]
   Nyckelord :HR8799; Planet formation; Protoplanetary disks; Giant planets; Astronomy; Migration; Dynamics; Physics and Astronomy;

   Sammanfattning : In the thriving field of exoplanet research new discoveries are made all the time, and while most of the observed systems can be explained with classical planet formation models - some are much harder to explain. When stars form they are often surrounded by the remaining material of the nebulae they formed from. LÄS MER