Letters of Intent received in 2018

LoI 2020-2025
Non-GA Symposium: Magnetars and Beyond: The Quest for a Unified Neutron Star Scenario

Date: 7 September 2020 to 12 September 2020
Location: Venice, Palazzo Franchetti, Sala Portego, Italy
Contact: GianLuca Israel (gianluca.israel@inaf.it)
Coordinating division: Division D High Energy Phenomena and Fundamental Physics
Co-Chairs of SOC: Gian Luca Israel (INAF OA Roma)
Roberto Turolla (Dept. of Physics and Astronomy)
Silvia Zane (MSSL-UCL London)
Nanda Rea (Institute of Space Sciences, CSIC-IEEC)
Co-Chairs of LOC: Roberto Turolla (Dept. of Physics and Astronomy)
Silvia Zane (MSSL-UCL London)



- Galactic neutron stars, population synthesis.
- Links among diverse neutron star classes.
- Magneto-thermal evolution of neutron stars.
- Neutron stars magnetic field.
- Multiwavelength magnetar observations.
- Magnetar formation and their progenitors.
- Magnetar magnetospheres.
- Neutron stars as sources of gravitational waves.
- Magnetar-GRB connection.
- Future perspectives, missions and observational facilities



Neutron stars are born when a massive star ends its life in a core-collapse supernova explosion. All the physical conditions in these
objects are extreme. With central densities 5-10 times larger than the nuclear density, they represent one of the densest forms of matter in the universe. Moreover, neutron stars are the strongest known magnets. Their surface magnetic field, normally in the TeraGauss range, may reach values 1000 times higher in the so-called "magnetars", largely exceeding the critical field above which effects of nonlinear quantum electrodynamics become important. Therefore, neutron stars provide excellent laboratories to probe the properties of matter under conditions that can not be reproduced in ground-based experiments, or met in other astrophysical environments. Multi-wavelength observations have changed dramatically our vision of neutron stars, very much the same way a panchromatic view of the world compares to a black and white one. Or iginally discovered as pulsars, Isolated Neutron Stars (INSs) have now been observed across the entire electromagnetic spectrum, up to high-energy gamma-rays, and they exhibit a complex and much diverse phenomenology. In particular, high energy
observations unveiled peculiar classes of radio silent INSs, whose existence would have passed unnoticed otherwise, e.g. the Soft Gamma Repeaters (SGRs), Anomalous X-ray Pulsars (AXPs), Central Compact Objects (CCOs) in supernova remnants and X-ray Dim Isolated Neutron Stars (XDINSs).
It is presently unknown whether the phenomenology we observe in these different sources and our classification thereof reflects differences in intrinsic properties (for example progenitors with different masses, or different spin periods and/or magnetic field strengths at birth) or is a consequence of evolution. Explaining the different INSs manifestations, the physics behind them, and the relations among different INSs types is one of the most chal lenging goals in compact objects astrophysics and offers the key to the ultimate understanding of the endpoints of massive star evolution.
The most extreme INS subgroup is that of AXPs and SGRs. Both these types of sources undergo periods of erratic bursting activity, and the latter even emit giant flares, hyper-energetic events which can outshine for a fraction of a second the entire Galaxy. There is strong evidence that these flares excite torsional mode oscillations in the neutron star crust that could provide unique insight into the equation of state of these highly-magnetized stars. These sources are, in fact, currently believed to be the strongest magnets in the cosmos, hosting NSs with a magnetic field as large as B~1E14- 1E15 G. More than 30 years elapsed since the first spectacular giant flare was detected on March 5th 1979 from SGR 0526-66, the first observational indication of the existence of a magnetar. Since then, the neutron star research, both observational and theoretical, has flourished. In particular, the advent of the latest generation space- and ground-based observatories has largely impacted on our knowledge of magnetars and other classes of neutron stars. All these objects are now studied in the whole electromagnetic spectrum, with ground-based radio, optical and infrared telescopes, and with the latest X-ray and Gamma ray observatories (including INTEGRAL, Chandra, XMM-Newton, Swift, Suzaku, NuSTAR, Fermi, NICER and AGILE).
The recent, spectacular detection of the gravitational wave signal, and of its electromagnetic counterpart, coming from the coalescence of two neutron stars opened a completely new window in neutrons star studies. The future holds great promises for neutron star astrophysics, with the launch of Athena+ among the confirmed high energy missions, and of the forthcoming multiwavelength facilities such as, among others, SKA, CTA, E-ELT. A key role in this research effort will be played by present (advanced LIGO/VIRGO), and future (LISA) gravitational wave detectors. The launch of the first ever X-ray polarimentric satellite (IXPE in 2021) and the forthcoming eXTP mission will add a new dimension to the observations of neutron stars.
For all these reasons it is our opinion that the time is ripe for gathering together both observers and theoreticians working in this field, in a meeting that will focus on breakthrough research linking astrophysics, particle physics and condensed matter physics. In this respect, we believe an IAU meeting is an ideal framework, offering a stimulating environment to review the current state of the art, to promote fruitful collaborations and discuss future perspectives.

Confirmed SOC members are: GianLuca Israel (Italy), Roberto Turolla (Italy), Silvia Zane (UK), Nanda Rea (Spain/Netherlands), Metthew Baring (USA), Dong Lai (USA), Samar Safi-Harb (Canada), Jeremy Heyl (Canada), Maxim Lyutikov (USA), Dima Yakovlev (Russian Federation), Sandro
Mereghetti (Italy), Rosalba Perna (USA)