Web-page maintained by isima@ucsc.edu. Last updated Oct. 1, 2009.

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UCSC

ISIMA 2014 Conference: Gravitational Dynamics

CITA Toronto, June 30th - July 4th 2014.

The ISIMA conference is hosted in the first week of the ISIMA program, and features invited pedagogical lectures in the morning, with afternoon contributed talks presenting state-of-the-art research on the program topic. Participation to the ISIMA conference is open to everyone who wishes to attend.

The morning lectures are video-recorded, and meant for a broad audience. The afternoon talks are typically 20-25 minutes long each, and present the latest developments in the field. All presentations are published online, please click on the link to access them.

More detail about the upcoming conference will be posted as the organization of the program proceeds.

Scientific Program

Sunday 6/29:

  • 5 pm - 7 pm: Informal gathering at the Bedford Academy on 36 Prince Arthur Avenue. This is a nice pub with an outdoor patio. Come and meet fellow ISIMA participants in a relaxed atmosphere! Note that we were not able to book a private room for this ISIMA event, but look for people with name tags to find your colleagues.

Monday 6/30: Room 134 in the McLennan Labs (see map ). Please be at the doors between 8:45 and 9:15 at the latest to be sure to be allowed in, the buildings are otherwise closed because the university is closed on that day. If you are stuck outside, please call numbers sent by email.

  • 9:00 am - 9:30 am: Welcome words and basic information
  • 9:30 am - 1:00 pm: Lectures.
  • 1:00 pm - 2:30pm: Lunch break at Baldwin St.
  • 2:30 pm - 3:30pm: Orientation; Visit of campus;
  • 3:30 pm - 4:00 pm: Afternoon Break
  • 4:00 pm - 5:30 pm: Project presentations

Tuesday 7/1: Room 134 in the McLennan Labs (see map ). Please be at the doors between 8:45 and 9:00 to be sure to be allowed in, the buildings are otherwise closed because the university is closed on that day. If you are stuck outside, please call numbers sent by email.

  • 9:00 am - 12:30 pm: Lectures
  • 12:30 pm - 2:00 pm: Lunch break
  • 2:00 pm - 3:30 pm: Contributed talks
  • 3:30 pm - 4:00 pm: Afternoon Break
  • 4:00 pm - 5:30 pm: Project discussion time.

Wednesday 7/2: CITA seminar room, 1318A McLennan Labs (see map )

  • 9:00 am - 12:30 pm: Lectures
  • 12:30 pm - 2:00 pm: Lunch break, project discussion time
  • 2:00 pm - 3:30 pm: Contributed talks
    • Alice Quillen: Three-body resonances
    • Mark Gieles: The life cycles of globular clusters in tidal fields
    • Florent Renaud: Galactic tides on star clusters: rocking the cradle and nailing the coffin.
  • 3:30 pm - 4:00 pm: Afternoon Break
  • 4:00 pm - 5:30 pm: Poster session and/or project discussion time.

Thursday 7/3: CITA seminar room, 1318A McLennan Labs (see map )

  • 9:00 am - 12:30 pm: Lectures
  • 12:30 pm - 2:00 pm: Lunch break, project discussion time
  • 2:00 pm - 3:30 pm: Contributed talks
  • 3:30 pm - 4:00 pm: Afternoon Break
  • 4:00 pm - 5:30 pm: Project discussion time.
  • 7:00 pm - late: Conference dinner at Asian Legend.

Friday 7/4: CITA seminar room, 1318A McLennan Labs (see map )

  • 9:00 am - 12:30 pm: Lectures
  • 12:30 pm - 2:00 pm: Lunch break, project discussion time
  • 2:00 pm - 3:30 pm: Contributed talks
  • 3:30pm - 4:00 pm: Afternoon Break
  • 4:00 pm - 5:30 pm: Project discussion time.
  • 5:30 pm: Closing remarks

 

 

Morning Lectures:

 

Doug Lin: Introductory Lecture.

Lecture : PDF presentation (large file!)

Video recording part 1.

Video recording part 2.

Video recording part 3.

 

Douglas Heggie: Lectures on Globular Cluster Dynamics.

PDFs for lectures 1, 2 and 3 : Snapshot models; Semi-analytical or simplified models; N-Body simulations.

Lecture 1: Video recording part 1.

Lecture 1: Video recording part 2.

Lecture 2: Video recording part 1 (audio only)

Lecture 2: Video recording part 2

Lecture 3: Video recording part 1

Lecture 3: Video recording part 2

 

David Merritt: Dynamics of galactic nuclei


Scott Tremaine: Lectures on Planetary Dynamics.

Lecture 1: video recording (unfortunately incomplete)

Lecture 2: video recording part 1.

Lecture 2: video recording part 2.

Lecture 2: video recording part 3.

Lecture 3: video recording


 

Afternoon Talks:

 

Sukanya Chakrabarti: Deciphering the dynamical echoes of the Milky Way satellites on the galactic disk.

PDF presentation

 

Elena d'Onghia: Self-perpetuating spiral arms in disk galaxies

PDF presentation

Video recording

 

Mark Gieles: The life cycles of globular clusters in tidal fields.

PDF presentation

Video recording part 1

Video recording part 2

 

Douglas Heggie: Star cluster dynamics: what we don't know.

PDF presentation

 

Andreas Kupper: Modeling the debris of globular clusters

PDF presentation

Video recording

 

Yoram Lithwick: Lessons from Kepler

PDF presentation

Video recording:

 

Man Hoi Lee: Did our solar system lose a giant planet?

PDF presentation

Video recording

 

David Merritt: Relativistic loss-code dynamics.

PDF presentation

Hagai Perets: Formation of irregular satellites

PDF presentation

Video recording

 

Alice Quillen: Three-body resonances

PDF presentation

Video recording

 

Florent Renaud: Galactic tides on star clusters: rocking the cradle and nailing the coffin.

Abstract: Coupling between scales occurs through a wide diversity of physical processes like turbulence, magnetic fields, feedback. Among them, gravity and its differential form, the tidal field, are present at all scales. The tidal field of interacting galaxies appears to be compressive over large volumes and coincide with the properties of the starburst activity. I propose a new theory to explain the enhancement of star formation in extended volumes, involving compressive tides and the cascade of this energy down to small scales via compressive turbulence. Using hydrodynamical simulations, I found a strong correlation between the tidal trigger and the starburst, leading to the formation of massive star clusters, probably the progenitors of globular clusters. When formed in the early Universe, at least a fraction of these clusters need to survive the galactic interactions to be detected at present day. Using the direct code Nbody6tt, based on Aarseth's Nbody6, we follow the evolution of a population of star clusters in a merger and note that the galactic collisions have no direct impact on the dissolution of clusters. By changing their orbit however, they leave an imprint on the long term evolution of these stellar objects.

PDF presentation

 

Yanqin Wu: Dynamics of large-N planetary systems

PDF presentation

Video recording part 1

Video recording part 2