This seminar is an informal forum where members of the DIANA group meet to discuss topics of interest. We meet on a weekly basis. The programme for these meetings will be advertised below, and by email.
If you wish to be added to (or removed from) our email list, please contact tobias.beran@univie.ac.at: subscribe or unsubscribe.
The the seminar takes place every Friday at 09:45 am in SE 07 and streamed via moodle and will be announced by email weekly.
Anyone interested is welcome to attend.
| Date | Speaker | Title |
|---|---|---|
| 04.10.2024 | Scheduling | |
| 11.10.2024 | Tobias Beran | Timelike curvature bounds in Lorentzian length spaces AbstractI will introduce several notions of timelike curvature bounds in Lorentzian length spaces and prove their equivalence. I will also introduce the new four-point condition and prove its equivalence. Let's see ho far I will get... |
| 18.10.2024 | Masoumeh Zarei | Positive curvature conditions and Ricci flow AbstractSince the introduction of Ricci flow by Hamilton in 1982, it has been a fundamental problem to understand the evolution of metrics and their curvature properties under the flow. While positive scalar curvature and 2-positive curvature operator are preserved in all dimensions, there exist infinitely many dimensions where certain curvature conditions lying in between are not preserved. In this talk, I will present some examples which admit metrics with different curvature conditions and discuss the evolution of their metrics under the Ricci flow. This is based on joint works with David González- Álvaro. |
| 25.10.2024 | Karim Mosani | Geometry and topology of trapped photon region in stationary axisymmetric black hole spacetimes AbstractIn Schwarzschild spacetime with positive mass $M$, there exist (unstable) circular orbits of trapped null geodesics at the Schwarzschild radius $r=3M$, outside the black hole horizon at $r=2M$. These orbits fill a three-dimensional submanifold $S^2\times \mathbb R$ called the photon sphere of the Schwarzschild spacetime. In general, a region in spacetime that is a union of all trapped null geodesics is called the Trapped Photon Region (TPR) of spacetime. In this seminar, we will consider three models of stationary, axisymmetric (sub-extremal and extremal) black hole spacetimes: Kerr, Kerr-Newman, and Kerr-Sen. We will see that, unlike the TPR of Schwarzschild spacetime, the TPR in such spacetimes is not a submanifold of the spacetime in general. However, its canonical projection in the (co-)tangent bundle is a five-dimensional submanifold of topology $SO(3)\times\mathbb R^2$. This result has potential applications in various problems in mathematical relativity. The talk is based on the paper by Cederbaum and Jahns (2019), where they prove the result in Kerr spacetime, and by Cederbaum and myself (under preparation), where we extend this result to the remaining two abovementioned spacetimes. |
| 08.11.2024 | Daniele Semola | The large scale structure of 4-manifolds with nonnegative Ricci curvature and Euclidean volume growth AbstractThanks to Gromov’s pre-compactness theorem and the work of Cheeger and Colding, any complete n-manifold with nonnegative Ricci curvature and Euclidean volume growth is asymptotic to a family of cones at infinity in the pointed Gromov-Hausdorff sense. When $n=4$ a naive argument neglecting all the regularity issues suggests that the sections of these cones at infinity are positively Ricci curved and hence homeomorphic to spherical space forms, by Hamilton’s work. I will discuss joint work with Elia Bruè and Alessandro Pigati where we make this argument rigorous. |
| 15.11.2024 | Marta Sálamo | Lagrangian surfaces AbstractA symplectic manifold is a pair $\left(X^{2n},\omega\right)$, where $X^{2n}$ is a smooth manifold and $\omega$ is a differential 2-form such that $\operatorname{d}\omega=0$ and $\omega^n>0$, known as the symplectic form. This simple definition gives rise to a broad area in geometry and topology with many connections to other disciplines such as classical mechanics, low-dimensional topology or algebraic and complex geometry. Among the many objects that one can study in this setting, we find the Lagrangian submanifolds. These are those submanifolds $L$ of half the ambient dimension on which the symplectic form vanishes identically on each tangent space of $L$. The study of Lagrangian submanifolds is a central topic in symplectic topology that can tell us a great deal about the symplectic manifold $(X,\omega)$. There are many interesting questions one can ask about Lagrangian submanifolds. In this work, we will study one of these.We study the minimal genus question for a symplectic rational 4-manifold $(X,\omega)$, which asks, for a given $A\in H_2(X;\mathbb Z_2)$, what are the possible topological types of non-orientable Lagrangian surfaces in the class $A$; and specially, what is the maximal Euler number, or, equivalently, the minimal genus. We start by ensuring that 2-homology classes can be represented by a non-orientable surface. Next, we are able to proof that, when having a symplectic structure in our manifold, these surfaces representing the homology classes can be taken to be non-orientable embedded Lagrangians. In this setup, the minimal genus question arises, and we study a partial answer to this question for rational 4-manifolds. We will see that if a homology class $A\in H_2(X;\mathbb Z_2)$ is realised by a non-orientable embedded Lagrangian surface $L$, then $\mathcal{P}(A)=\chi(L)\ \operatorname{mod}\ 4$, where $\mathcal{P}(A)$ is the Pontrjagin square of $A$. We will briefly discuss the problem for the zero class, and prove the main result of the essay for non-zero classes, which states the reciprocate for some symplectic structures in the case of rational 4-manifolds. |
| 22.11.2024 | Kharanshu Solanki | Strong curvature naked singularities from gravitational collapse AbstractA spacetime singularity is called Tipler strong if the volume form acting on independent Jacobi fields defined by causal geodesics vanishes as the singularity is approached. Such a singularity is accompanied by a notion of strong Ricci curvature growth along incomplete geodesics. On the other hand, a naked singularity is one that can be identified by the past-incompleteness of causal geodesics. A key question concerning the cosmic censorship debate is whether there exists "generic" initial data that can collapse to a naked singularity in finite time. This question was initially addressed in the well known works of Datt (1938) and Oppenheimer and Snyder (1939) for homogeneous dust data. An alternative approach was developed by Joshi and Dwivedi (1993) for inhomogeneous dust. The idea is to consider the geodesic equation in the limit of the singularity. This yields an algebraic equation, and the polarity of its roots indicates whether the singularity is naked or not. One then imposes the sufficient condition for the existence of a Tipler strong singularity as given by Clarke and Królak (1985), in order to guarantee that any body approaching the naked singularity will be crushed to zero size, and thereby rendering these singularities as physically interesting. For spherically symmetric collapse, the formation of strong curvature naked singularities can be characterized by a single parameter related to the mass profile and physical radius of the collapsing matter shell. I will present the generalizations of this line of work in the following directions: (i) generalization to higher dimensions, (ii) generalization to all type-I matter fields. |
| 29.11.2024 | Miguel Prados | Spaces of geodesics |
| 06.12.2024 | Samuël Borza | Sub-Lorentzian geometry |
| 13.12.2024 | Carl Rossdeutscher | Rigidity of singularity theorems |
| 10.1.2025 | Joe Barton | tba |
| 17.1.2025 | Inés Vega | decay on exterior of BHs |
| 24.1.2025 | Vanessa Ryborz | |
| 31.1.2025 | Jona Röhrig | Gromov Hausdorff compactness |