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Phase Transitions in Astrophysics, from ISM to Planets
from
Sunday, 7 May 2017 (09:00)
to
Friday, 2 June 2017 (18:00)
Monday, 1 May 2017
Tuesday, 2 May 2017
Wednesday, 3 May 2017
Thursday, 4 May 2017
Friday, 5 May 2017
Saturday, 6 May 2017
Sunday, 7 May 2017
Monday, 8 May 2017
11:30
The Magnetized and multiphase ISM as seen by Planck
-
Andrea Bracco
The Magnetized and multiphase ISM as seen by Planck
Andrea Bracco
11:30 - 12:30
Room: 122:026
Tuesday, 9 May 2017
11:00
Smooth Particle MHD, method, expectatives and strategies
-
Federico Stasyszyn
Smooth Particle MHD, method, expectatives and strategies
Federico Stasyszyn
11:00 - 12:00
Room: 122:026
I will introduce Smoothed Particle Hydrodinamics as a numerical method, focussing particularly on the pros and cons when simulating ISM and accretion discs. Additionally I will comment on MHD implementations that currently successfully implemented.
15:30
Python installation tutorial
Python installation tutorial
15:30 - 16:00
Room: 122:026
Wednesday, 10 May 2017
10:00
Practical Python for Researchers (1st part)
-
Simon Candelaresi
Practical Python for Researchers (1st part)
Simon Candelaresi
10:00 - 10:45
Room: 122:026
11:00
Practical Python for Researchers (2nd part)
-
Simon Candelaresi
Practical Python for Researchers (2nd part)
Simon Candelaresi
11:00 - 12:00
Room: 122:026
15:30
Practical Python for Researchers (3rd part): discussion
Practical Python for Researchers (3rd part): discussion
15:30 - 16:30
Room: 122:026
Thursday, 11 May 2017
11:00
On the different kinds of superfluid vortices in the interior of neutron stars
-
Giacomo Marmorini
On the different kinds of superfluid vortices in the interior of neutron stars
Giacomo Marmorini
11:00 - 12:00
Room: 122:026
Friday, 12 May 2017
11:00
Critical phenomena, nonlinear dynamics and the formation and detection of planets
-
John Wettlaufer
Critical phenomena, nonlinear dynamics and the formation and detection of planets
John Wettlaufer
11:00 - 12:00
Room: 122:026
Saturday, 13 May 2017
Sunday, 14 May 2017
Monday, 15 May 2017
11:00
50 years of thermal instability : what have we learned ? what are the new questions ?
-
Marc-Antoine Miville-Deschenes
50 years of thermal instability : what have we learned ? what are the new questions ?
Marc-Antoine Miville-Deschenes
11:00 - 12:00
Room: 122:026
Tuesday, 16 May 2017
15:30
Formation and evolution of filaments in the interstellar medium
-
Evangelia Ntormousi
Formation and evolution of filaments in the interstellar medium
Evangelia Ntormousi
15:30 - 16:30
Room: 122:026
Wednesday, 17 May 2017
11:00
The HI turbulence: temperature distribution, buildup of molecular clouds, and ineffective stellar feedback
-
Snezana Stanimirovic
The HI turbulence: temperature distribution, buildup of molecular clouds, and ineffective stellar feedback
Snezana Stanimirovic
11:00 - 12:00
Room: 122:026
15:30
Clustering and dynamic decoupling of dust grains in turbulent molecular clouds
-
Lars Mattsson
(
Nordita
)
Clustering and dynamic decoupling of dust grains in turbulent molecular clouds
Lars Mattsson
(
Nordita
)
15:30 - 16:30
Room: 122:026
Thursday, 18 May 2017
11:00
Shining Light on the Dark ISM
-
Joanne Dawson
Shining Light on the Dark ISM
Joanne Dawson
11:00 - 12:00
Room: 122:026
Friday, 19 May 2017
11:00
The Dark Milky Way: Probing our Galaxy’s Hidden Gas
-
Van Hiep Nguyen
The Dark Milky Way: Probing our Galaxy’s Hidden Gas
Van Hiep Nguyen
11:00 - 11:20
Room: 122:026
Many studies have proved the existence of the “dark interstellar medium” (dark ISM) which is not detected by traditional radio emissions from atomic hydrogen (HI) and carbon monoxide (CO) molecules. In recent years, OH has emerged as a powerful indicator of dark-ISM. In this study, we use HI and OH data from the Arecibo Millennium survey (Heiles and Troland 2003) which observed absorption and emission pairs towards 79 extragalatic radio continuum sources. The Λ-doubling transitions of ground-state OH at 1665.402 and 1667.359 MHz were observed along with HI towards 48 of the 79 survey positions. By newly reducing this unpublished data, OH absorption was detected in 23 lines- of-sight, we find that the OH 1665 and 1667 lines satisfy the optically thin assumption with the optical depth τ less than 0.25 and they are in general not in Local Thermal Equilibrium. By comparing the thermal dust data from Planck satellite (Release 1.2) and the Sloan Digital Sky Survey (Schlafly et al. 2011) with HI data from Millennium survey, we confirm the tight linear correlations between optical depth τ353, dust radiance R, reddening E(B-V) and the total proton column density N(H). We estimate the molecular hydrogen column densities N(H2)=1⁄2[N(H)-N(HI)] from these linear relationships and hence the OH abundance ratio XOH=N(OH)/N(H2), for which few literature measurement exist. The XOH ratios derived from the three N(H) proxies are consistent and appear to be constant around 5.0×10-6. Since these results are obtained in a wide ranges of longitude l and latitude b with some sightlines through the Galactic plane, it suggests that OH main lines are excellent tracers of molecular gas in the interstellar medium including regimes where the usefulness of CO is compromised.
11:30
Feedback and interactions from low-mass stars in the Coronet cluster
-
Mara Elizabeth Pelayo Baldárrago
Feedback and interactions from low-mass stars in the Coronet cluster
Mara Elizabeth Pelayo Baldárrago
11:30 - 11:50
Room: 122:026
Saturday, 20 May 2017
Sunday, 21 May 2017
Monday, 22 May 2017
11:00
Phase Transition Dynamics of ISM: The Formation of Molecular Clouds and Galactic Star Formation
-
Shu-ichiro Inutsuka
Phase Transition Dynamics of ISM: The Formation of Molecular Clouds and Galactic Star Formation
Shu-ichiro Inutsuka
11:00 - 12:00
Room: 122:026
Magnetohydrodynamics of interstellar medium is remarkably different from that of simple barotropic gas owing to the phase transitions between cold phase and warm phase (and hot phase) that trigger variety of instabilities. Identifications of distinct instabilities in various stages provide us important clues for understanding the saturation levels of turbulent energies and rates of formation and destruction of cold clouds, such as HI clouds and molecular clouds. Recent high- resolution magneto-hydrodynamical simulations of phase transition dynamics with cooling/heating and thermal conduction have shown that the formation of molecular clouds requires multiple episodes of supersonic compression. This finding enables us to create a new scenario of molecular cloud formation as the interacting shells or bubbles in galactic scale, which explains many observational properties such cloud-to-cloud velocity dispersions, accelerating star formation, and very low star formation efficiencies in filamentary molecular clouds. We estimate the ensemble-averaged growth rate of individual molecular clouds, and predict the associated cloud mass function. Cloud-cloud collisions as a mechanism for forming massive stars and star clusters can be naturally accommodated in this scenario. This explains why massive stars formed in cloud-cloud collisions follows the power-law slope of the mass function of molecular cloud cores repeatedly found in low-mass star forming regions.
Tuesday, 23 May 2017
11:00
Fragmentation of a Filamentary Molecular Cloud Permeated by Perpendicular Magnetic Field
-
Tomoyuki Hanawa
Fragmentation of a Filamentary Molecular Cloud Permeated by Perpendicular Magnetic Field
Tomoyuki Hanawa
11:00 - 12:00
Room: 122:026
15:30
Effects of the multi-phase character of the interstellar medium on the Galactic dynamo
-
Oliver Gressel
(
Nordita
)
Effects of the multi-phase character of the interstellar medium on the Galactic dynamo
Oliver Gressel
(
Nordita
)
15:30 - 16:30
Room: 122:026
Wednesday, 24 May 2017
11:00
Reduced gas accretion onto Super-Earths and ice giants
-
Michiel Lambrechts
Reduced gas accretion onto Super-Earths and ice giants
Michiel Lambrechts
11:00 - 12:00
Room: 122:026
15:30
Geophysical test for habitability in icy ocean worlds
-
Steven Vance
Geophysical test for habitability in icy ocean worlds
Steven Vance
15:30 - 16:30
Room: 122:026
Thursday, 25 May 2017
11:00
Some aspects of protoplanetary disc formation and evolution
-
Patrick Hennebelle
Some aspects of protoplanetary disc formation and evolution
Patrick Hennebelle
11:00 - 12:00
Room: 122:026
Friday, 26 May 2017
11:00
Riddles from the AU Microscopii system
-
Alexis Brandeker
Riddles from the AU Microscopii system
Alexis Brandeker
11:00 - 12:00
Room: 122:026
AU Microscopii is a nearby red dwarf, belonging to the beta Pictoris moving group. Like beta Pic, AU Mic is famous for its big, edge-on debris disk. Recent high-resolution, multi-epoch imaging of the system has revealed baffling features in the disk in the form of clumps moving at super-Keplerian speed out from the system. Currently, there is no satisfactory explanation for the origin and dynamics of the clumps. In this talk I will review the current facts and hypotheses, and propose a way forward towards solving this mystery.
14:00
Discussion on NASA Europa mission
Discussion on NASA Europa mission
14:00 - 15:00
Room: 122:026
Saturday, 27 May 2017
Sunday, 28 May 2017
Monday, 29 May 2017
11:00
Jupiter internal structure and the first Juno results
-
Yamila Miguel
Jupiter internal structure and the first Juno results
Yamila Miguel
11:00 - 12:00
Room: 122:026
15:30
Characterisation of Exoplanets, how to understand their mass, radius, and atmospheric composition
-
Pascal Tremblin
Characterisation of Exoplanets, how to understand their mass, radius, and atmospheric composition
Pascal Tremblin
15:30 - 16:30
Room: 122:026
Tuesday, 30 May 2017
11:00
Effect of Phase Transitions on Turbulent Transport
-
Igor Rogachevskii
(
Ben-Gurion University of the Negev
)
Effect of Phase Transitions on Turbulent Transport
Igor Rogachevskii
(
Ben-Gurion University of the Negev
)
11:00 - 12:00
Room: 122:026
Wednesday, 31 May 2017
11:00
Detection and characterization of planets around M Dwarfs
-
Mario Damasso
Detection and characterization of planets around M Dwarfs
Mario Damasso
11:00 - 12:00
Room: 122:026
M dwarfs are optimal targets to search for potentially habitable planets in the solar neighborhood through the photometric transit method and the analysis of radial velocity timeseries. Spanning almost all the low- mass spectral range, "breaking news" terrestrial planets have been found around some nearby M dwarfs, and they will be the primary follow-up targets for further characterization in the near future. After introducing the state-of.-the-art techniques used to detect those planets, I will focus on some of the most promising by highlighting in particular the challenges posed by stellar activity and spectroscopical observational sampling for a proper characterization of their bulk composition.
15:30
Disentangling the structures in debris disks: Planets or just gas?
-
Areli Castrejon
Disentangling the structures in debris disks: Planets or just gas?
Areli Castrejon
15:30 - 15:50
Room: 122:026
Thursday, 1 June 2017
11:00
Implementing a Radially Efficient Poisson Equation Solver to Investigate Tidal Downsizing
-
Vincent Carpenter
Implementing a Radially Efficient Poisson Equation Solver to Investigate Tidal Downsizing
Vincent Carpenter
11:00 - 11:20
Room: 122:026
11:30
Convection on Jupiter's icy moons as a consequence of tidal forces
-
Leonardo Cassarà
Convection on Jupiter's icy moons as a consequence of tidal forces
Leonardo Cassarà
11:30 - 11:50
Room: 122:026
14:00
Solving radiation and hydrodynamics using a moments model
-
Argel Ramírez Reyes
Solving radiation and hydrodynamics using a moments model
Argel Ramírez Reyes
14:00 - 14:20
Room: 122:026
14:30
Presentation of an all-Mach regime solver
-
Thomas Padioleau
Presentation of an all-Mach regime solver
Thomas Padioleau
14:30 - 14:50
Room: 122:026
Friday, 2 June 2017
