Frank P. Pijpers
Imperial College Press, 2006 .
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Name: Frank P. Pijpers
Email: F.Pijpers _AT_ imperial.ac.uk
Fax: +44 20 7594 7772
Phone: +44 20 7594 7661
I used to work for the Space and Atmospheric Physics group at Imperial
College (London, England), and before that in the
Center based in the Astronomy Group
of the University of Aarhus (Denmark).
Before that I used to work in the Uppsala
Astronomical Observatory (Sweden), and at
Mary and Westfield College (now QMUL) before that.
Dynamics of stellar atmospheres
Circumstellar flows in evolved stars (and in YSOs)
Research interests :
(Directly from the ADS you can obtain an up to date
listing (restricted to astronomical journals) of
all, or just
- Waves, Convection & Turbulence
- Inversion & Image Reconstruction :
- (MNRAS 307, 659) (1999)
- Lect. Notes in Earth Sc.
92, ``Methods and Applications of Inversion'', Eds. Hansen, Jacobsen,
Mosegaard, 241 (2000)
- Look here for the IMA which
organised a winter school on inverse problems in 1995 for which this
was written. This has now appeared in :
IMA Volumes in Mathematics and its Applications 90, "Inverse problems in
wave propagation" eds. G. Chavent, G. Papanicolaou, P. Sacks, W. Symes,
Springer, New York, 1997. (Also available as pdf version)
- An application of the SOLA method on adaptive optics images of IR
emission of vibrationally excited molecular hydrogen in Orion.
(Proceedings Cargese conference,
- The interferometric determination of the radius of the nearby
star tau Ceti : (A & A
Gas dynamics in AGNs (reverberation mapping)
Time series analysis (gravitational lens time delays)
- The SOLA method is presented in
(A & A 281, 231) (1994)
- A SOLA-based method for 2-D rotational inversions is
(MNRAS 279, 498) (1996)
- for the proceedings of the IAU symposium 181, I wrote this .
- For solar rotation inversions one can use either frequency splittings or
a-coefficients. This paper shows relationships between them
(A & A 326, 1235) (1997).
- It is possible to determine the solar gravitational quadrupole
moment helioseismically. This paper shows how and gives a value
(MNRAS 297, L76)
- It is possible to do tomographic (3-D) seismic imaging of structures
just below the visible surface of the Sun. However, standard ray-tracing
techniques are flawed. This paper describes a better way using the Rytov
approximation (A & A 412, 257) (2003).
Lecture course material :
The sun is oscillating in many different pulsation modes which deform
it slightly. Here are two shown with an exaggerated vertical scale and
unrealistic colours. On the left is an L=8 M=4 spherical harmonic eigenmode,
on the right is an L=9 M=9 Spherical Harmonic eigenmode.
The solar rotation rate is shown here as a contour and grey scale plot
The darker the background, the more uncertain the determination of the
rotation rate. The contours are iso-rotation contours, labelled with
the rotation rate in nHz.
A passing interest in maps and projections has produced this page
Last updated 14 Dec 2006