CAMAP project
P.I. of CAMAP Project: Miguel A. Aloy Torás
Project full title: CAMAP: Computer aided modeling of astrophysical plasma
Grant agreement no.: 259276
Duration: 60 months
CAMAP is an Starting Independent Researcher Grant funded by the European Research Councill
Link to the News of University of Valencia
Link to a recent price: Premio IDEA 2011.
Contents

Project Summary:
In a broad sense, this project will be aimed at obtaining a deeper insight into the physical processes taking place in astrophysical magnetized plasmas, which involve a broad range of length and time scales. To study these scenarios the PI will employ different numerical codes as virtual tools that enable me to experiment on virtual laboratories (computers) with distinct initial a...nd boundary conditions, in a fully analogous way to the experiments that can be done in an actual laboratory. Among the kind of sources the PI is interested to consider, the PI outlines the following:
GammaRay Bursts (GRBs), extragalactic jets from Active Galactic Nuclei (AGN), magnetars and collapsing stellar cores.
A number of important questions are still open regarding the
fundamental properties of these astrophysical sources. The complete
description of the collimation and acceleration of astrophysical
jets is still being elucidated.
The composition, highenergy emission, and the mechanisms by which jets propagate from their formation sites to the locations where they are observed is a subject of active scientific debate. Predicting source dynamics and gravitational waveforms is important to understand hopedfor observations in the current generation of groundbased, gravitational wave detectors, and essential to achieve design sensitivity in future spacebased detectors. Additionally, there are analytical issues on the formalism in relativistic dynamics that are not completely resolved, particularly in the covariant extension of resistive magnetohydrodynamics.
All these problems are so complex that only a computational approach is feasible.
The PI plans to study them by means of (Magneto)Hydrodynamics (MHD) numerical simulations with a suitable coupling with the dynamics of populations of nonthermal emitting particles. Most of these astrophysical plasmas are relativistic (e.g., GRBs, AGN jets). Thus, they must be treated with a suitable Special or General Relativity approach.
The virtual laboratory the PI plans to develop will therefore be fully equipped with the most modern algorithms to cope with Special Relativistic MHD (SRMHD) or General Relativistic MHD (GRMHD) fluids. Other scenarios can be appropriately described by a classical or Newtonian MHD approach; hence the virtual lab will also be prepared for that. A principal focus of the project will be to assess the relevance of magnetic fields in the generation, collimation and ulterior propagation of relativistic jets from the GRB progenitors and from AGNs. More generally, the PI will pursue the goal of understanding the process of amplification of seed magnetic fields until they become dynamically relevant, e.g., using semiglobal and local simulations of representative boxes of collapsed stellar cores.
A big emphasis will be put on including all the relevant microphysics (e.g. neutrino physics), nonideal effects (particularly, reconnection physics) and energy transport due to neutrinos and photons to account for the relevant processes in the former systems.
A milestone of this project will be to end up with a numerical tool that enables us to deal with General Relativistic Radiation Magnetohydrodynamics problems in Astrophysics.
Why is it CAMAP groundbreaking?
Because of the diversity of time and length scales, so far we have only models for different stages in the gammaray burst (GRB) phenomenon.
I will try to obtain a consistent model to explain gammaray bursts from the collapse of massive stellar cores to the late afterglow.
Stateoftheart 
COLLAPSE 
Stellar core collapse from presupernova models
including (some) of the following:
Bfields, GR, microphysics, 3D, vtransport 
OUTFLOW 
Adhoc model of the central engine 
hypercreatingBH + initial B
(strenght + topology) 
Jet injection conditions 
Jet propagation: AMR, (ideal) (G)R(M)HD,
estimate flow conditions at transparency 
RADIATION 
Assumed ejecta structure, kinematic models, analytic or
simplified emission models 



 Magnetorotational core collapse from presupernova models in full (time evolving) GR, including microphysics, and (simplified) !transport.
 Collapse followed beyond BHformation, until a hyperaccreting BH forms.
 Bfield consistently computed from the evolution of the presupernova core.
 Propagation of the jet in GRRMHD until it reaches transparency.
 Consistent calculation of the observational signature (radiation).
Extensions: 3D, improved !transport, more emission processes (IC), etc.


Backup strategies
Among our goals, we also pretend to improve on our previous work. Even if everything else fails, this might allow us to perform highlevel science and obtain cuttingedge results (employing well tested methodology):
 Increasing dimensionality (computer scientists + increase in computing power):
 From 2D to 3D in progenitors of GRBs: jet stability, mass entrainment.
 From 1D to 2D in internal shocks: account for the lateral expansion, transition from early
afterglow to late afterglow, efficiency of the model
 Including magnetic fields where we had neglected them before:
 In progenitors of longGRBs: effects of adhoc fields on the propagation and on the observational fingerprint of jets.
 Inferring the ejecta magnetization in the prompt GRB phase and in the early afterglow.
 Numerical study of relativistic (magneto)fluid instabilities. E.g.: RayleighTailor instabilities in decelerating shells and its implication for GRBs.
 Using realistic magnetospheric models and studying the emission properties of the quasi periodic oscillations in the tail of giant flares of SGRs.
CAMAP a multidisciplinary proposal
CAMAP team
Person 
Expertise 
Codes 
Miguel A. Aloy (PI)
(dedication: 75%) 
RMHD, RRMHD, relativistic flows, stellar core collapse 
GENESIS 
Martin Obergaulinger 
MHD, Bfield amplification in PNSs, stellar core collapse, vtransport 
AENUS 
Pablo Cerdá Durá 
Dynamical evolution in full GR, GRMHD, stellar core collapse 
CoCoNuT 
Petar Mimica 
RMHD, Radiative Processes, relativistic flows 
GENESIS, SPEV 
 CAMAP project relies on the interaction between postdocs which share a common expertise in numerical methods for magnetohydrodynamics.
 We request a Ph.D student from this project, but we expect to attract one or two additional ones (UV funds, Spanish FPI, USA Fulbright, German DAAD, etc.).
 Nicolas DeBrye (Grisolia Fellow)
 Jesús Rueda (Grisolia Fellow)
 Carlos Cuesta (Master Student)
 Sergio Miranda
CAMAP Legacy
 This project is aimed at obtaining a deeper insight into the physical processes taking place in astrophysical objects hosting plasma that can be modeled as a fluid, among them, I outline GRBs, AGN jets and compact objects.
 Understand the role of the magnetic field in the dynamics of these sources.
 When/Where nonideal effects are relevant?
 We may try to bridge the gap between stellar corecollapse and the production of relativistic outflows and obtain a selfconsistent picture from collapse to the observational signature (full Einstein, microphysics, transport, emission).
 What is the jet composition?
 How do the outflows collimate/accelerate in a dynamically evolving spacetime?
 Characterization of the mechanism to build dynamically important Bfields from tiny seed values, and of the preferred field topology.
 Gravitational waveforms (stellar corecollapse, outflows). Needed to extract signals from the "detectable noise" in groundbased and spacebased detectors.
 We will develop a number of numerical tools to deal with astrophysical sources where the physics can be is dominated by (nonideal) (relativistic) (magneto) HD.
