The department is located at:
Ångström Laboratory, Polacksbacken, Lägerhyddsvägen 1.
Here's how to find us.
The seminars are available in several formats:
- Web: http://www.physics.uu.se/en/seminars/calendar
- iCal: http://www.physics.uu.se/sv/calendar/all/ical
- RSS-feed: http://www.physics.uu.se/en/seminars/upcoming/rss.xml
Information about Astronomy and Space Physics seminars
- Usual seminar time is Thursday, 14.00 sharp (45 min talk + 15 min discussion)
- Usual seminar room is Hiorters rum, floor 3, house 7
- Group meetings: Planets: Tue 15-16, IRFU: Wed 11-12, Galaxies: Fri 15-16, Stars: Fri 14-15
- Seminars at other Swedish institutes: Stockholm, Lund, Onsala
- Past and present IRFU seminars: 1996-present day
- Comments or inquiries regarding Astronomy and Space Physics seminars should be directed to the
seminar organizers (Andreas Korn and Eric Stempels).
Information about Nuclear and Particle Physics seminars
- Usual seminar time is Thursday, 15.15 (45-50 min talk + 10-15 min discussion)
- Usual seminar room is 12167, floor 2, southern end of house 1
- Comments or inquiries regarding Nuclear and Particle Physics seminars should be directed to the seminar organizer (Andrzej Kupsc and Richard Brenner).
Information about Theoretical Physics seminars
- Usual seminar time is Wednesday, 13.15-14.15
- Usual seminar room is Oseenska rummet, floor 3 house 7
- Past seminars: 2003-
- Comments or inquiries regarding the Theoretical Physics seminars should be directed to the seminar organizer (Thomas Klose)
Information about Applied Nuclear Physics seminars
- Comments or inquiries regarding the Applied Nuclear Physics seminars should be directed to the seminar organizer (Anna Davour)
Information about Materials Theory seminars
- Usual seminar time is Friday, 12.00-12.45
- Usual seminar room is Å80101, floor 0 house 8
- Comments or inquiries regarding the "Materials Theory Friday Seminars" should be directed to the seminar organizer (Sumanta Bhandary)
Last updated 2014-05-14 14:14.
The NASA Kepler survey has identified numerous Earth-size planets transiting other stars, and limited Doppler radial velocity measurements hint that many of these are primarily made of heavy, refractory elements, i.e. are "rocky". However, we have no direct measurements of the composition of these planets. The photospheres of Sun-like stars offer indirect information because the stars and protoplanetary disks have a common origin, and material accreted from a disk can change the abundances in the relatively thin convection zones of these stars. A strong correlation between giant planet occurrence and stellar metallicity has proved robust to scrutiny, but the underlying mechanism is unclear.
The presentation is given as part of the Neutron Resonance Analysis School I attended in 2011. I will present the general evaluation process; describe the resonance parameters and how they are represented in the ENDF format. Also, a brief description of the general theoretical models used in the analysis of neutron resonance data - R-matrix theory (the single-level Breit-Wigner, the multi-level Breit Wigner and Reich Moore approximation) for the resolve region and the Hauser-Feshbach theory for the unresolved resonance region will be covered. Finally, the Doppler broadening of the single level Breit-Wigner formalism for resonance absorption will be presented.