One of the greatest current unsolved problems in physics is whether gravitation, the least understood of the fundamental "forces", is universally Newtonian in the classical limit. Even the nature of gravitation is unclear: is it a force in the physical sense (with an exchange particle), an apparent force resulting from the distortion of space-time or just an emergent phenomenon due to entropy differences as suggested by Verlinde? Whatever the physical origin of gravitation, the empirical formulation of how a body is accelerated as a result of the mass-distribution around it can be applied to study the formation and evolution of galaxies. There are two hypothesis available for computational study now:
The hypothesis that gravitation is Newtonian, as derived empirically based on Solar-system data only, has been embedded in Einstein's interpretation of gravitation as being a geometric space-time distortion. This interpretation leads to departures from observed motions of astronomical objects when extrapolated to the scales of galaxies and beyond. These departures are usually interpreted to be due to the existence of new elementary (dark matter) particles and due to the hitherto not understood dark energy which needs to dominate the energy content of the Universe and is increasing with time.
By taking into account the new dynamics data that became available on the scales of galaxies in the late 1970s, Milgrom generalised the classical law of gravitation. The hypothesis that gravitation is Milgromian simplifies galactic astrophysics because no additional dark matter is needed and galaxies become fully self-gravitating systems based on their baryonic matter content only.
The following challenges emerge in view of the two hypotheses:
Dark matter remains elusive: There is no room for dark matter particles within the standard model of particle physics. The decades long searches in space, underground and at the Large Hadron Collider for these putative particles have all been failures, and dynamical friction on the motions of satellite and larger galaxies due to the expansive dark matter haloes is not evident, as if dark matter particles are non-existent. In addition, already early cosmological computations based on the Newtonian hypothesis with dark matter have turned up major problems (e.g. the angular momentum problem, the missing satellite problem, amongst many) which have never been solved convincingly, while new problems keep emerging (the satellite planes problem, the radial acceleration relation problem, amongst many). Can this hypothesis nevertheless be made to be consistent with the observational data?
The Milgromian hypothesis on the other hand, while accounting for many of the above problems, is a non-linear theory and thus poses computational challenges. It has, until recently and due to a variety of reasons, not been applied to the problem of galaxy formation and it is therefore unclear if galaxies will emerge to look like the observed population in this approach.
With this meeting we aim to foster a discussion between the scientists who have been studying galaxies and cosmology in these two fundamentally different hypotheses. The aim is to achieve an exchange notably also on the technical challenges in applying both hypotheses to computational astrophysics problems in view of recent advances in understanding stellar populations, which are important for quantifying feedback processes.
Please register by sending an email to
firstname.lastname@example.org with subject "registration"
and let us know if you would like to give a presentation and
if you do not want your name to be listed on the
participants list (EU GDPR 2018). The default is that your
name will be displayed. Registrations will be accepted by
students at a research institution (we may need to ask for a
reference letter or two) and/or researchers who have at
least one peer-reviewed original research
publication on a topic related to this meeting. There will
be no invited or overview talks as such.
If you wish to give a talk, then please also send us a title and abstract when you register (we are accepting abstracts until the end of May). We will try our best to fulfil all requests for a talk. The proposed talks ought to be on the topic of testing Newtonian vs Milgromian gravitation and/or on technical aspects related to galaxy formation and evolution (e.g., the numerical treatment of supernova explosions, of the multiphase inter stellar medium and chemical enrichment), or on observational topics related to the Newtonian vs Milgromian gravitational problem.
The talk lengths are envisioned to be between 20 and 40 minutes, depending on how many talks are requested. There will be about 30-40 talks in total, and we are aiming to allow for ample discussion time of each presentation.
The organisers are aiming to not raise a registration fee, but financial assistance for participants will not be available.
The programme will become available here. We expect the following outline: Monday morning to Friday afternoon (5 full days), with 3, 2 and 3 talks per day (coffee and lunch breaks in between) and a general discussion at the end. A welcome reception on the evening of the first day is planned. A conference dinner is planned for Wednesday evening.
So far ...
SOC: Indranil Banik (chair, Bonn), Hosein Haghi (Zanjan), Pavel Kroupa (co-chair, Bonn, Prague), Oliver Müller (Strasbourg), Xufen Wu (Hefei), Akram Hasani Zonoozi (Bonn, Zanjan)
LOC: Christa Boersch, Moritz Haslbauer, Nils Wittenburg