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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.

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

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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