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Seminars

May 2018
Mon Tue Wed Thu Fri Sat Sun
1 2 3
ESP Online Seminar: Interactions between pre-existing and emerging magnetic flux systems observed with IRIS (S. Guglielmino)

from 11:00 to 12:00

 4 5 6
7 8
Solar and Stellar Group Seminar: The solar dynamo: Inferences from observations (R. Cameron)

from 11:00 to 12:00

 9
Solar and Stellar Group Seminar: Uniqueness results for inverse problems given the imaginary part of Green's function (A. Agaltsov)

from 11:00 to 12:00

S3 Seminar: Non-linearity calibration for CMOS Sensors (K. Sant)

from 14:00 to 14:30

S3 Seminar: Inverse Problems in Asteroseismology (E. Bellinger)

from 14:30 to 15:00

S3 Seminar: Detecting Exomoons (K. Rodenbeck)

from 15:15 to 15:45

 10 11 12 13
14 15
Solar and Stellar Group Seminar: Reconstructing the coronal magnetic field, a model comparison (T. Wiegelmann)

from 11:00 to 12:00

 16
S3 Seminar: Polar magnetic fields as observed by SUNRISE (A. Prabhu)

from 14:30 to 15:00

 17 18 19 20
21 22 23
S3 Seminar: Investigation of lunar slope instabilities using Convolution Neural Networks (V. Bickel)

from 14:00 to 14:30

S3 Seminar: How cool are starspots? (M. Panja)

from 14:30 to 15:00

 24 25 26 27
28 29 30
S3 Seminar: Solar surface flows of emerging active regions (N. Gottschling)

from 14:00 to 14:30

S3 Seminar: The blue planet - origin of water on Earth (M. Fischer)

from 14:30 to 15:00

S3 Seminar: Optimal averaging for helioseismic measurements using the singular value decomposition (M. Pourabdian)

from 15:00 to 15:30

 31

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Welcome to the MPS

Welcome to the Max Planck Institute for Solar System Research
Welcome to the Max Planck Institute for Solar System Research
Rosetta: Cometary jets at sunriseRosetta: Cometary jets at sunrise
Rossby waves on the SunRossby waves on the Sun
InSight successfully launchedInSight successfully launched

Welcome to the Max Planck Institute for Solar System Research

Our immediate cosmological surroundings are the research focus of the Max Planck Institute for Solar System Research: the solar system with its planets and moons, its comets and asteroids, and of course the Sun. The aim of the scientists is not only to theoretically model the workings of the solar system and simulate them on the computer, however. In close cooperation with their engineer colleagues, they also develop and build scientific instruments that investigate these celestial bodies. To do this, the institute collaborates with international space agencies such as NASA and ESA on numerous missions.

This department investigates the deep interior, the surfaces, atmospheres, ionospheres, and magnetospheres of planets and their moons, as well as comets and asteroids. The department contributes to important space missions such as the ESA mission Rosetta, which investigates the comet Churyumov-Gerasimenko; the NASA mission Dawn, which investigates the dwarf planet Ceres; and the NASA mission InSight, which is planned to investigate the deep interior of Mars.

Department Planets and Comets

This department investigates the deep interior, the surfaces, atmospheres, ionospheres, and magnetospheres of planets and their moons, as well as comets and asteroids. The department contributes to important space missions such as the ESA mission Rosetta, which investigates the comet Churyumov-Gerasimenko; the NASA mission Dawn, which investigates the dwarf planet Ceres; and the NASA mission InSight, which is planned to investigate the deep interior of Mars.
The focus of this department is the solar interior, the solar atmosphere, the solar magnetic field, the heliosphere, and the interplanetary medium, as well as solar radiation and solar energetic particles. The balloon-mission Sunrise, a balloon-borne solar observatory, is managed by this department. The mission investigates our central star from a height of about 35 km above sea level. In addition to several other participations in space missions, the department significantly contributes to the ESA mission Solar Orbiter, which is scheduled for launch in 2017.

Department Sun and Heliosphere

The focus of this department is the solar interior, the solar atmosphere, the solar magnetic field, the heliosphere, and the interplanetary medium, as well as solar radiation and solar energetic particles. The balloon-mission Sunrise, a balloon-borne solar observatory, is managed by this department. The mission investigates our central star from a height of about 35 km above sea level. In addition to several other participations in space missions, the department significantly contributes to the ESA mission Solar Orbiter, which is scheduled for launch in 2017.

Methods of helioseismology are used in this department to explore the interior mechanisms of our star. The key to this are the turbulent convection flows in the solar interior, which cause the Sun to vibrate in millions of different ways. Similar methods are used for investigating the magnetic fields of solar-like stars. The department hosts the German Data Center for SDO, the only German data center of the NASA mission Solar Dynamics Observatory.

Department Solar and Stellar Interiors

Methods of helioseismology are used in this department to explore the interior mechanisms of our star. The key to this are the turbulent convection flows in the solar interior, which cause the Sun to vibrate in millions of different ways. Similar methods are used for investigating the magnetic fields of solar-like stars. The department hosts the German Data Center for SDO, the only German data center of the NASA mission Solar Dynamics Observatory.

All activity phenomena in the Sun and other stars originate from their magnetic fields, which arise due to a hydromagnetic dynamo that converts kinetic energy into magnetic form. Even the solar dynamo remains enigmatic due to the extreme complexity of phenomena related to it. Observations of other stars provide important constraints on the stellar dynamo mechanism(s). The work of the group aims at combining these observations with theory and 3D numerical simulations to gain better understanding of the solar and stellar dynamos.

Max Planck Research Group: Solar and Stellar Magnetic Activity

All activity phenomena in the Sun and other stars originate from their magnetic fields, which arise due to a hydromagnetic dynamo that converts kinetic energy into magnetic form. Even the solar dynamo remains enigmatic due to the extreme complexity of phenomena related to it. Observations of other stars provide important constraints on the stellar dynamo mechanism(s). The work of the group aims at combining these observations with theory and 3D numerical simulations to gain better understanding of the solar and stellar dynamos.
Radiation from the Sun makes Earth a habitable planet. Fluctuations in the solar radiative output are therefore likely to affect the climate on Earth, but establishing both how the output of the Sun varies and how such variations influence Earth's climate have proved tricky.  Increased amounts of data from the Sun and about the climate on Earth over recent years means that rapid progress is being made.  This work is aimed at understanding solar variability and the Sun's influence on the Earths' climate.

Minerva-Group: Solar Variability and Climate

Radiation from the Sun makes Earth a habitable planet. Fluctuations in the solar radiative output are therefore likely to affect the climate on Earth, but establishing both how the output of the Sun varies and how such variations influence Earth's climate have proved tricky.  Increased amounts of data from the Sun and about the climate on Earth over recent years means that rapid progress is being made.  This work is aimed at understanding solar variability and the Sun's influence on the Earths' climate.
Age is a fundamental property of stars. It is an essential tool to understand phenomena such as the evolution of stars, planetary systems, and the Galaxy. However, age is the most poorly known property of a star. Asteroseismology, the study of the internal structure of stars through stellar oscillations, offers the opportunity to estimate the ages of stars with much higher accuracy than before. Combining space observations with ground-based spectroscopy, the group determines the ages of thousands of stars with unprecedented precision.

Max Planck Research Group and ERC Starting Grant:
Stellar Ages and Galactic Evolution

Age is a fundamental property of stars. It is an essential tool to understand phenomena such as the evolution of stars, planetary systems, and the Galaxy. However, age is the most poorly known property of a star. Asteroseismology, the study of the internal structure of stars through stellar oscillations, offers the opportunity to estimate the ages of stars with much higher accuracy than before. Combining space observations with ground-based spectroscopy, the group determines the ages of thousands of stars with unprecedented precision.

The SOLVe group aims at connecting the related studies of solar and stellar variability based on the models originally developed for the Sun.

ERC Starting Grant: Connecting Solar and Stellar Variabilities (SOLVe)

The SOLVe group aims at connecting the related studies of solar and stellar variability based on the models originally developed for the Sun. [more]
The group focusses on understanding the activity of comets and asteroids. This leads us to better understand how comets and asteroids evolve with time, and what the properties of their surfaces and sub-surface layers are.

ERC Starting Grant: Activity of Comets and Asteroids

The group focusses on understanding the activity of comets and asteroids. This leads us to better understand how comets and asteroids evolve with time, and what the properties of their surfaces and sub-surface layers are.
In order to learn something about the Sun or other stars we usually have to rely on indirect observations, i.e. we can only observe effects of an unknown quantity. This group works on the corresponding inverse problems to reconstruct the unknown causes from the observed effects. A particular focus is on the reconstruction of convection fields from measurements of oscillations of the solar surface.

Max Planck Fellow Group: Inverse Problems

In order to learn something about the Sun or other stars we usually have to rely on indirect observations, i.e. we can only observe effects of an unknown quantity. This group works on the corresponding inverse problems to reconstruct the unknown causes from the observed effects. A particular focus is on the reconstruction of convection fields from measurements of oscillations of the solar surface. [more]
 
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