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MAGNESIA SIGNED

The impact of highly magnetic neutron stars in the explosive and transient Universe

Total Cost €

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EC-Contrib. €

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Partnership

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 MAGNESIA project word cloud

Explore the words cloud of the MAGNESIA project. It provides you a very rough idea of what is the project "MAGNESIA" about.

phases    model    errors    magnesia    3d    explosive    innovative    galaxy    put    hampers    variety    imperative    super    works    first    ultra    limits    suggested    stars    physics    double    rotational    magnetars    fundamental    modeling    mergers    powering    largely    numerical    models    populations    wavy    inhibited    flares    fast    expertise    showed    evolution    supernovae    nuclear    observations    energy    computational    flaring    observational    knowing    luminous    infer    cope    interpretations    hypernovae    power    release    window    wave    radio    census    gamma    quantitative    constraints    birth    highest    nor    computation    rates    possibly    ray    systematic    bursts    measured    star    population    sound    discovery    period    events    enormous    sources    transient    synthesis    universe    lacking    dipolar    magnetar    pulsar    tracers    densities    gravitational    combining    magnetic    despite    neutron    pulsars    band    spin   

Project "MAGNESIA" data sheet

The following table provides information about the project.

Coordinator
AGENCIA ESTATAL CONSEJO SUPERIOR DEINVESTIGACIONES CIENTIFICAS 

Organization address
address: CALLE SERRANO 117
city: MADRID
postcode: 28006
website: http://www.csic.es

contact info
title: n.a.
name: n.a.
surname: n.a.
function: n.a.
email: n.a.
telephone: n.a.
fax: n.a.

 Coordinator Country Spain [ES]
 Total cost 2˙263˙148 €
 EC max contribution 2˙263˙148 € (100%)
 Programme 1. H2020-EU.1.1. (EXCELLENT SCIENCE - European Research Council (ERC))
 Code Call ERC-2018-COG
 Funding Scheme ERC-COG
 Starting year 2019
 Duration (year-month-day) from 2019-06-01   to  2024-05-31

 Partnership

Take a look of project's partnership.

# participants  country  role  EC contrib. [€] 
1    AGENCIA ESTATAL CONSEJO SUPERIOR DEINVESTIGACIONES CIENTIFICAS ES (MADRID) coordinator 2˙263˙148.00

Map

 Project objective

The gravitational wave window is now open. It is then imperative to build quantitative models of neutron stars that use all the available tracers to constrain fundamental physics at the highest densities and magnetic fields. The most magnetic neutron stars, the magnetars, have been recently suggested to be powering a large variety of explosive and transient events. The enormous rotational power at birth, and the magnetic energy they can release via large flares, put the magnetars in the (yet) hand-wavy interpretations of gamma-ray bursts, the early phases of double neutron star mergers, super-luminous supernovae, hypernovae, fast radio bursts, and ultra-luminous X-ray sources. However, despite knowing about 30 magnetars, we are lacking a census of how many we expect within the pulsar population, nor we have robust constraints on their flaring rates. The recent discovery of transient magnetars, of magnetar-like flares from sources with measured low dipolar magnetic fields and from typical radio pulsars, clearly showed that the magnetar census in our Galaxy is largely under-estimated. This hampers our understanding not only of the pulsar and magnetar populations, but also of them as possibly related to many of Universe’s explosive events. MAGNESIA will infer a sound Magnetar Census via an innovative approach that will build the first Pulsar Population Synthesis model able to cope with constraints/limits from multi-band observations, and taking into account 3D magnetic field evolution models and flaring rates for neutron stars. Combining expertise in multi-band observations, numerical modeling, nuclear physics, and computation, MAGNESIA will solve the physics, the observational systematic errors, and the computational challenges that inhibited previous works, to finally constrain the spin period and magnetic field distribution at birth of the neutron star population.

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