Peter Hauschildt

Peter H. Hauschildt
Professor of Astronomy
Hamburger Sternwarte
Gojenbergsweg 112
21029 Hamburg
Phone: +49 40 428 38 8512
Fax: +49 40 428 38 8598
Email: yeti "AT" hs.uni-hamburg.de
(note: all mail labelled 'SPAM' will
be automatically deleted!)

I am Professor for Astronomy at the Hamburger Sternwarte (observatory), which is part of the Department of Physics of the University of Hamburg. I served as Dept. Chair from 01/2014 until 12/2015, as Deputy Dept. Chair for 3.5 years and as Managing Director of the observatory for 3 years.

My main area of research is the modeling of stellar and planetary atmospheres using computer simulations with our PHOENIX code. This is a large scale supercomputing application, my group regularily uses large parallel supercomputers that can be found in the top 10 of the world's fastest supercomputers. My CV is available as PDF file and I also have a list of publications available (PDF, infrequently updated, please use ADS for up-to-date information!). I am a member of the Lothar Collatz Center for Computing in Science. My group has often opportunities for Bachelor & Master theses in the field of theoretical and computational astrophysics, please contact me for more information.

Vorlesungsinfos

For current class information please use the STINE pages of the university.

Astronomy program information

Please check out the web pages of the observatory for a FAQ list.

My main research interests are (not necessarily in this order):

(More information can be found on the PHOENIX homepage)

3D radiative transfer algorithms and their implementation.
continue the development & verification of PHOENIX/3D.
The atmospheres and spectra of novae, M dwarfs & giants, Brown Dwarfs, L/T dwarfs, T Tauri's, SNe, basically everything that radiates.
Irradiation of planets and secondaries of CVs
Analyses of Nova, M/L/T dwarf & giant, Brown Dwarf, T Tauri, and SN spectra.
The detailed physics of nova spectra, in particular line blanketing and NLTE effects.
Numerical methods for NLTE and radiative transfer calculations.
Line formation, blending and blanketing in (relativistically) expanding atmospheres.
Radiative transfer in relativistically expanding, spherical atmospheres.
Detailed NLTE calculations for extremely large model atoms.
Effective numerical methods to treat 100's of millions spectral lines individually with detailed profiles.
Molecular line opacities.
Line broadening in very cool stars.
Finishing the next versions of the M/L/T-O dwarf and nova model grids.
Models for Stellar Winds
Keeping PHOENIX/1D and PHOENIX/3D alive and happy (currently at version 19.02 with a host of new and beautiful arcane bugs!).

More information is available on the PHOENIX page

My friend and long time collaborator France Allard has passed away. Here are a few thoughts.

This page was last modified by PHH on 12.07.2023

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