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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.

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

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

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 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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