Dr
Yuri cavecchi
(University of Southampton - Princeton University)
When a neutron star accretes from a low mass companion, the fluid that
accumulates on the surface of the compact object can burn
unstably. The result of the thermonuclear runaway is the Type I
bursts: X-ray flashes that last for tens to hundreds of seconds. The
lightcurves of the bursts encode information about the mass and radius
of the neutron star. These can be used to put constraints...
Dr
Ornella Juliana Piccinni
(University of Rome 'Sapienza' - INFN)
Continuous waves (CW) are still undetected gravitational wave signals emitted by rotating neutron stars, isolated or in binary systems. The estimated number of isolated neutron stars in our Galaxy is 10^8-10^9. Information provided by electromagnetic observations is crucial to constrain the signal parameter space, lower the computational cost of a CW search and increase the number of potential...
Dr
Domenico Logoteta
(University of Pisa)
I will report on the calculation of a new equation of state (EOS) derived
from Chiral Effective Field Theory (ChEFT) for nucleonic and hyperonic
matter. A new feature of this EOS is the inclusion in a consistent way
of the effect of hyperonic three-body forces.
I will focus in particular on the three-body force originating from the
interaction between two nucleons and...
Prof.
Diego F. Torres
(ICREA & Institute of Space Sciences (ICE, CSIC))
In this talk I introduce a model based on only 3 parameters and a global normalization scale that is able to describe the varied spectra of gamma-ray/X-ray pulsars known across 7 orders of magnitude in energy. This model provides at once an answer of what process is behind the emission spectra and how the spectral variety arises. It explains why we have detected sub-exponential cutoffs in...
Dr
Alice Borghese
(Anton Pannekoek Institute, University of Amsterdam)
Magnetars are the strongest magnets we know of. Their X-ray emission is powered by the instabilities and decay of their huge magnetic field (~10^14-10^15 G). They are characterized by unpredictable and variable bursting activity in the X-/gamma ray regime, often accompanied by enhancements of the persistent X-ray flux. These events are called outbursts. In this talk, I will present new results...
Dr
Joeri van Leeuwen
(ASTRON / U. Amsterdam)
Apertif is a highly innovative receiver system that is currently starting operations on the Westerbork Synthesis Radio Telescope. Its factor 40 increase in field-of-view allows astronomers to survey the sky at 1.4 GHz with an unprecedented combination of sensitivity and speed. At high time resolution this enables deep searches for millisecond transients over the entire Northern hemisphere. In...
Mr
Alessandro Montoli
(Università degli Studi di Milano & INFN)
In the interior of a mature neutron star, the differential rotation of the neutron superfluid star with respect to the normal component allows to store angular momentum, which is released during a pulsar glitch. Recent studies show how it is in principle possible to estimate pulsar masses from observations related to their timing properties. In this talk we will compare the mass estimates made...
Jaroslaw Dyks
(Copernicus Astronomical Center)
Observed radio pulsar polarization exhibits a range of complicated phenomena which
cannot be explained by the rotating vector model. These
include strong distortions of a polarization angle curve and high levels of
circular polarization V. Properties of the circular polarization are quite
peculiar: V tends to peak in coincidence with orthogonal
mode transitions, and can have both signs...
Mr
Crispin Agar
(Jodrell Bank Centre for Astrophysics)
Pulsar polarisation is key to understanding the emission mechanism. Some radio pulsars exhibit puzzling polarisation properties and variability at the single-pulse level. PSR B0031-07 is one such radio pulsar, which shows rapid changes in position angle that are apparently modulated as the star rotates, and periodical changes are seen from pulse to pulse. It is demonstrated that this...
Ms
Claudia Gonzalez-Boquera
(Univeristy of Barcelona)
A precise determination of the core-crust transition is necessary when modelling neutron
stars for astrophysical purposes.
The core-crust transition in this work is studied with finite-range nuclear interactions using the dynamical approach for detecting the instability of the matter in the core against density perturbations.
Also, we analyze the correlation of the transition properties,...
Prof.
Luca Del Zanna
(University of Florence)
Compact objects, and neutron stars in particular, are characterised by strong magnetic fields that are crucial to explain the high-energy emission from the sources. These magnetic fields may be subject to complex evolution inside the hosting relativistic plasma, like dynamo or chiral processes amplifying initial seed fields in early stages, or dissipative reconnection events in thin current...
Dr
Anthea Francesca Fantina
(Grand Accélérateur National d'Ions Lourds (GANIL))
X-ray observations of soft X-ray transients in quiescence suggest the existence of heat sources in the crust of accreted neutron stars. The heat is thought to be released by electroweak and nuclear processes triggered by the burying of ashes of X-ray bursts.
In this talk, the heating in the crust of accreting neutron stars will be discussed. In particular, the importance of nuclear physics...
Ms
Marcella Wijngaarden
(University of Southampton)
One of the challenges affecting the study of neutron star cooling is obtaining the interior temperature from observations of surface emission. The relation between surface temperature and interior temperature is set by the heat conducting properties of the thin outer envelope, which are highly sensitive to chemical composition. Most state-of-the-art cooling models consider the envelope to...
Mr
Vincent Morello
(University of Manchester)
We will present the latest data on PSR J2251$-$3711, a radio pulsar with a 12.1-second spin period discovered in the SUPERB survey at Parkes. Combined with the recent unexpected discovery of PSR J0250$+$5854, which has an even longer 23.5-second spin period, the possibility of finding even slower radio emitting pulsars is now wide open. Not only do these objects challenge our understanding of...
Prof.
Bruno Giacomazzo
(University of Trento)
I will present fully general relativistic simulations of binary neutron star mergers employing a new zero-temperature chiral effective field theory equation of state (EOS), the Bombaci-Logoteta (BL) EOS, and compare with simulations using the older GM3 EOS, which is based on standard relativistic mean-field theory. I will provide a detailed analysis of the dynamics, with focus on the...
Dr
Kate Maguire
(Queen's University Belfast)
Observations and theoretical modelling of the first confirmed neutron star merger event, GW170817, have allowed us to probe for the first time the electromagnetic signatures of this catastrophic event. I will present an overview of the extensive multi-wavelength follow-up that was obtained for the 'kilnova' event that occurred with GW170817 (and any others that may have occurred by the time of...
Sabrina Schäfer
(Technische Universität Darmstadt, Institut für Kernphysik)
We investigate the impact of different properties of the nuclear equation of state in core-collapse supernovae, with a focus on the proto-neutron star contraction and its impact on the shock evolution. To this end, we introduce a range of equations of state that vary the nucleon effective mass, incompressibility, symmetry energy, and nuclear saturation point. This allows us to point to the...
Dr
Violetta Sagun
(CENTRA, Instituto Superior Técnico)
We apply the novel equation of state, which includes the surface tension contribution induced by the interparticle interaction and the asymmetry between neutrons and protons, to the study of neutron star properties. This equation of state is obtained from the virial expansion for the multicomponent particle mixtures that takes into account the hard-core repulsion between them. The considered...
Mrs
Cristina-Diana Ilie
(Jodrell Bank Centre for Astrophysics)
It is known that the radio signals of pulsars are highly linearly polarized, with the position angle (PA) of many pulsars changing across rotational phase in a way which is well described by the Rotating Vector Model (RVM). When the pulsar radiation propagates through the magnetized interstellar medium, it is affected by Faraday rotation. This results in a rotation of the plane of linear...
Mr
Alessio Marino
(Università degli studi di Palermo)
Since 1998, when the discovery of the first Accreting Millisecond X-ray Pulsar (AMXPs) SAX J1808.4-3658 occurred, the family of these sources kept growing on. Up to now, it counts 22 members, object of several studies due to the interesting, and sometimes puzzling, behavior shown by some of them. All AMXPs are transients with usually very long quiescence periods, implying that mass accretion...
Dr
Federico García
(AIM (Université Paris Diderot, CEA-Saclay, CNRS))
High mass X-ray binaries (HMXBs) are binary systems formed by a compact object (either a neutron star (NS) or a black hole) accreting from a massive stellar companion. These objects have gained new attraction after the discovery of gravitational waves emitted in compact object mergers of binary black holes and neutron stars. HMXBs are thought to be progenitors of these systems, depending on...
Dr
Niccolo' Bucciantini
(INAF - OA Arcetri)
Pulsars out of their parent SNR directly interact with the ISM producing so called Bow-Shock Pulsar Wind Nebulae. These have been directly observed from Radio to X-ray, and are found also associated to TeV halos, with a large variety of morphologies. They offer a unique environment where the pulsar wind can be studied by modelling its interaction with the surrounding ambient medium, in a...
Dr
Jason Hessels
(University of Amsterdam & ASTRON)
Fast radio bursts (FRBs) are millisecond-duration radio
flashes, apparently originating at cosmological distances. As such,
FRBs promise to provide a new view of extreme astrophysics in action -
with, e.g., potential insights into the deaths of massive stars,
particle acceleration, and the properties of the intergalactic medium.
While some FRBs may be associated with cataclysmic...
Dr
Maria Grazia Bernardini
(INAF - Osservatorio Astronomico di Brera)
Newly-born millisecond magnetars are competing with black holes as source of the gamma-ray burst (GRB) power, mainly with their rotational energy reservoir. In ten years of activity, Swift has provided compelling observational evidences supporting the magnetar central engine, as the presence of a plateau phase in the X-ray light curve, the extended emission in SGRBs and the precursor and...
Mr
Thomas Carreau
(Université Caen-Normandie)
The neutron star crustal EoS and transition point properties are computed within a unified meta-modeling approach.
The variational equations in the crust are solved within a Compressible Liquid Drop (CLD) approach, with surface parameters consistently optimized for each EoS set on experimental nuclear mass data.
When EoS parameters are taken from known Skyrme or RMF functionals, the...
Mr
Jay Vijay Kalinani
(University of Padova, Italy)
Recent detection of gravitational waves (GWs) from the merger of two neutron stars (NSs) by the Advanced LIGO-Virgo interferometers also accompanied by the observation of electromagnetic (EM) counterparts across the entire spectrum has opened the new field for multimessenger astrophysics with GW sources. Binary neutron star (BNS) merger events can be used as a laboratory to investigate the NS...
Magdalena Sieniawska
(Nicolaus Copernicus Astronomical Center PAS)
Using parametric equations of state (relativistic polytropes and simple quark bag model)
to model dense-matter phase transitions, we study global, measurable astrophysical
parameters of compact stars, such as their allowed radii and tidal deformabilities.
We also investigate the influence of stiffness of matter before the onset of the
phase transitions on the parameters of the possible...
Mr
Francesco Zappa
(Friedrich-Schiller-Universität Jena Theoretisch-Physikalisches Institut, Jena, Germany)
We give numerical relativity estimate of the luminosity peak of gravitational waves emitted during the coalescence of binary neutron stars. Our model is constructed from the CoRe-collaboration database and depends only on the main binary's parameters, allowing to make predictions of the luminosity of such events. Highest luminosity peaks are produced when the merger ends in a black hole that...
Dr
Paolo D'Avanzo
(INAF - Osservatorio Astronomico di Brera)
The spectacular detection of the first electromagnetic counterpart of a gravitational wave event detected by the LIGO/Virgo interferometers and originated by the coalescence of a double neutron star system (GW 170817) marked the dawn of a new era for astronomy. The (weak) short GRB 170817A associated to the GW event provided the long-sought evidence that at least a fraction of short GRBs are...
Mr
Péter Pósfay
(Wigner Researc Centre for Physics)
Description of dense nuclear matter rely on the experimental constraints
coming from the properties of "normal" nuclear matter found in nuclei and
observational data from neutron stars which consist of ultra dense nuclear matter.
In this presentation I show how the parameters of nuclear matter (effective nucleon mass, compressibility, and proton neutron asymmetry) influence the...
Prof.
Sergey Popov
(Sternberg Astronomical Institute, Lomonosov Moscow State University)
Several candidates for accreting magnetars have been proposed recently by different authors. Existence of such systems contradicts the standard magnetic field decay scenario where a large magnetic field of a neutron star reaches a few $\times 10^{13}$ G at agees $>$ Myr. Among other sources, the high mass X-ray binary 4U0114+65 seems to have a strong magnetic field around $10^{14}$ G. We...
Constança Providencia
(Universidade de Coimbra)
We analyse the effect of the density dependence of the symmetry energy on the hyperonic content of neutron stars within a relativistic mean field description of stellar
matter. For the $\Lambda$-hyperon, we consider parametrizations calibrated to $\Lambda$-hypernuclei. For the $\Sigma$ and $\Xi$-hyperons uncertainties that reflect the present lack of experimental information on $\Sigma$ ...
Ms
Kelly Gourdji
(Anton Pannekoek Institute)
On 17 August 2017, gravitational waves (GWs) from a binary neutron star inspiral (GW170817) were detected for the first time, by the Advanced LIGO and Advanced VIRGO GW detectors. This triggered an observing campaign of unprecedented scale that covered the full electromagnetic spectrum and launched the era of multimesseneger astronomy. Ongoing monitoring of the radio emission in particular,...
Dr
Jérôme Guilet
(CEA Saclay, Department of Astrophysics)
Extremely strong magnetic fields of the order of 10^15 Gauss are required to explain the properties of magnetars, the most magnetic neutron stars. Such a strong magnetic field is expected to play an important role for the dynamics of core-collapse supernovae, and in the presence of rapid rotation may power superluminous supernovae and hypernovae associated to long gamma-ray bursts. The origin...
Dr
Francisco Castillo
(Institute of Astrophysics (PUC Chile))
The study of the evolution of neutron star magnetic fields is likely to help us understand the connection between the different classes of NSs, which have magnetic fields of very different strengths, depending on their age. This observational evidence suggests that the NS magnetic field evolves in time. Numerous studies, both purely theoretical and numerical, have contributed to understand the...
Dr
Konstantinos Gourgouliatos
(Durham University)
I will review the ideas behind neutron star magnetic field evolution. The magnetic field of neutron stars can evolve in short (~seconds) and long (~kyr) timescales. The former is manifest in magnetar explosive activity, while the latter is most likely related to persistent thermal emission from strongly magnetised neutron stars. We can distinguish three main regions where magnetic field...
Dr
Samuel Lander
(N. Copernicus Astronomical Centre)
Stresses build up in a neutron star's crust as its magnetic field evolves, until the crust eventually yields. This occurs as a plastic deformation, and is believed to be responsible for coronal activity from magnetars. Existing simulations of crustal magnetic-field evolution assume, however, that the crustal lattice is fixed and never yields, meaning that the field evolves only under the...
Prof.
Sylvain Chaty
(Université Paris Diderot - CEA Saclay)
Most High Mass X-ray Binaries (HMXB) host a neutron star accreting from the intense stellar wind of a massive star. They have been revealed by a wealth of multi-wavelength observations, from X-ray to infrared domain. I will review here what these observations have brought to light about our knowledge of HMXB, and which part of HMXB still remains mysterious.
Intensive programs, including...
Dr
Domitilla de Martino
(INAF - Capodimonte Observagtory Naples)
We will discuss the multi-band orbital variability and long-term behaviour of millisecond pulsar binaries particularly of redback systems and transitional millisecond pulsars in the rotation-powered state to understand the role of pulsar spin down power in the intrabinary shock emission and irradiation of the companion.
Micaela Oertel
(LUTH, CNRS-Observatoire de Paris)
Neutrinos play an important role in compact star
astrophysics: neutrino-heating is one of the main ingredients in
core-collapse supernovae, neutrino-matter interactions determine the
composition of matter in binary neutron star mergers and have among
others a strong impact on conditions for heavy element nucleosynthesis
and neutron star cooling is dominated by neutrino emission except...
Dr
David E. Alvarez Castillo
(Joint Institute for Nuclear Research)
In this talk I will review the method of estimation of tidal deformabilities of compact stars and present results for pure hadronic
as well as hybrid stars that include the mass twins case. Then I will discuss the impact of the nuclear symmetry energy in
the determination of the compact star radius.In particular, the recent detection of gravitational radiation from the GW170817 event
shed...
Dr
Andrei Igoshev
(Technion - Israel Institute of Technology)
Using the most precise interferometric measurements of parallax and proper motion together with the rigorous statistical methods, we refined the natal kick velocity distribution for the neutron stars. The proper modelling of the natal kicks is essential to understand the formation of X-ray binaries, millisecond radio pulsars and double neutron stars (gravitational wave sources). We have found...
Ms
Alena Khokhryakova
(Lomonosov Moscow State University)
We discuss the possibility of detecting associated X-ray emission from sources of fast radio bursts with the eROSITA telescope onboard the Spektr-RG observatory. It is shown that during the four years of the survey program, about 300 bursts are expected to appear in the field of view of eROSITA. About 1% of them will be detected by ground based radio telescopes. For a total energy release...
Prof.
Armen Sedrakian
(Frankfurt Institute for Advanced Studies)
I will discuss the recent progress in understanding some of the properties of compact stars which feature hyperons, delta-resonances and quark matter. The discussion will include static properties of such stars and their cooling behaviour.
Prof.
Ian Jones
(University of Southampton)
A newly born magnetised neutron star can undergo free precession if its spin and magnetic axes are misaligned. The magnetic axis can then either tend to align or become orthogonal to the spin axis, depending upon a delicate interplay of magnetic spin-down torques and internal viscous dissipation. In this talk I will describe our modelling of this process, and how the distribution of...
Prof.
Leonardo Gualtieri
(University of Rome "La Sapienza")
Gravitational waves from compact binaries are probably the most promising probe of the behaviour of matter in the inner core of neutron stars. Recently the tidal deformability of neutron stars has been measured by LIGO/Virgo, leading to a reliable estimate of the radius and to constraints on the equation of state. I will discuss how these measurements can be made more accurate, providing...
Dr
Cristobal Espinoza
(Universidad de Santiago de Chile)
In this talk I will summarize our current understanding of pulsar glitches based on analyses of recent data. Aspects such as glitch size distributions, the time series of glitches, glitch rates, and glitch activity will be reviewed; and some selected particular cases will be discussed.
Dr
Marco Antonelli
(Nicolaus Copernicus Astronomical Centre of the Polish Academy of Sciences)
Nuclear superfluidity is thought to play a key role in the dynamics of isolated neutron stars. In particular, pulsar glitches offer a glimpse into the superfluid interior of a neutron star: within the currently accepted scenario these timing irregularities are explained in terms of the motion of quantized vortex lines that permeate the superfluid region.
To store the angular momentum which...
Dr
Alice Harding
(NASA Goddard Space Flight Center)
Recent progress in global simulation of pulsar magnetospheres is changing our models of pulsar particle acceleration, cascade pair production and high-energy emission. Simulation of a force-free pulsar magnetosphere 15-20 years ago marked a major advance in understanding the current closure and the structure of the wind. The first simulations of dissipative MHD pulsar magnetospheres with...
Dr
Federico Guercilena
(IKP - Tu Darmstadt)
We perform full GR simulations of binary neutron-star mergers em-
ploying three different nuclear-physics EOS, considering both equal-
and unequal-mass configurations, and adopting a leakage scheme to ac-
count for neutrino radiative losses. Using a combination of techniques,
we carry out an extensive and systematic study of the hydrodynamical,
thermodynamical, and geometrical properties...
Mr
Frank Chambers
(University of Amsterdam)
Accreting neutron stars (NS) can exhibit high frequency modulations in their lightcurves during thermonuclear X-ray bursts, known as burst oscillations. These frequencies can be offset from the NS spin frequency by several Hz (known independently) and can drift by 1-3 Hz. One plausible explanation is that a wave is present in the bursting ocean that decreases in frequency (in the rotating...
Mr
Stefano Ascenzi
(Gran Sasso Science Institute/INAF-Oar/INFN)
The observation of Gravitational Wave (GW) event (GW170817) and its electromagnetic counterpart in gamma rays (GRB 170817) and in optical and near-infrared (AT2017gfo) marked the beginning of the multimessenger astronomy with GWs. This event was also the first detection of a binary neutron star (BNS) coalescence as well as the first clear observation of a kilonova, an astrophysical transient...
Mr
Elia Giliberti
(Università degli Studi di Milano)
In accreting neutron stars (NSs), centrifugal forces can cause the failure of the crust. This event, called starquake, may produce a rotating mass quadrupole moment that allows the emission of gravitational waves (GWs). The angular momentum lost via GWs can balance the one gained from accretion, stopping the stellar spin-up. We use a Newtonian model, describing a compressible, stratified NS,...
Mr
Ankan Sur
(Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences)
The binary neutron star event GW170817 with its optical counterpart led to the first standard siren measurement of the Hubble constant $H_0$. This was possible due to a direct estimate of the luminosity distance from the gravitational-wave strain and a measurement of the redshift from the transient electromagnetic counterpart. Even in the absence of such a counterpart, we can statistically...
Mr
Zhivko Stoyanov
(Institute for Nuclear Research and Nuclear Energy, Bulgarian Academy of Sciences)
The r-process triggered by the decompression of ejected crustal materials from binary neutron star mergers has been recently confirmed by observations of the kilonova following the detection of gravitational waves from GW170817. Isolated neutron stars endowed with very high magnetic fields, so called magnetars, might be also at the origin of r-process nucleosynthesis since some material is...
Prof.
Dany Page
(Instituto de Astronomia, Universidad Nacional Autonoma de Mexico)
Neutron star low-mass X-ray binaries with transient accretion are unique systems to study the interior of neutron stars. During the accretion phase the crust of the neutron star is strongly heated and most of this heat flows into the core. During the quiescence phase the star relaxes back to thermal equilibrium and observation of this phase allows to map the physical properties of the stellar...
Prof.
Nils Andersson
(University of Southampton)
The observation of a large glitch in the Vela pulsar in 1969 initiated a discussion that is still – more than half a century later – ongoing. The general view is that the glitch phenomenon is linked to the presence of a superfluid component penetrating the neutron star crust. However, this remains (in many ways) a cartoon-level explanation. Quantitative modelling is a challenge. In this talk I...
Prof.
Michael Kramer
(MPI fuer Radioastronomie)
We are living in a golden era for testing gravitational physics with precision experiments. This talk will give a status of the field using a variety of tests with radio pulsars. It will highlight the use of multi-messenger information, which allows us to place the results in context of other experiments (including LIGO, EHT, etc). I will demonstrate how pulsars continue to provide unique...
Dr
William Newton
(Texas A&M University-Commerce)
We present the most extensive set of 3D, microscopic quantum calculations of nuclear pasta to date, under conditions relevant to the crusts of neutron stars, and spanning the current uncertainty in nuclear models. We show that quantum shell effects and the small differences in surface energies of different pasta configurations lead to a large number of local minima in their energy surfaces at...
Dr
Robert Ferdman
(University of East Anglia)
PSR J1913+1102 is a double neutron star system (DNS) discovered with the Arecibo radio telescope in the PALFA survey. With previous observing campaigns, we have determined that with its short orbital period of less than 5 hours, it is one of the most relativistic DNSs known. We have precisely determined the individual masses, which are the most asymmetric among compact DNS binaries. In this...
Dr
Miguel-Ángel ALOY
(University of Valencia)
Using numerical simulations in two and three dimensions, we investigate the collapse of the highly compact cores of high-mass stars with varying degrees of rotation and magnetic fields that are commonly considered progenitors of gamma-ray bursts (GRBs) within the collapsar or the proto-magnetar model. Our simulations aim to find the specific values of the magnetic field and its topology that...
Prof.
Paola Leaci
(Sapienza University and INFN)
Following the discoveries of transient gravitational-wave signals, more efforts and resources have been employed to detect continuous gravitational waves (CWs). These faint signals are emitted by asymmetric and quickly rotating neutron stars, both isolated and in binary systems, and are among the most interesting targets of the Advanced LIGO-Virgo detectors.
The search for this kind of...
Dr
Alessandro Papitto
(INAF Osservatorio Astronomico di Roma)
The magnetic field of most of the neutron stars in low mass X-ray binaries are much weaker than in younger systems such as neutron stars with a high mass companion, magnetars and most of the radio pulsars. Nonetheless, even a low magnetic field may have a significant impact on the flow of matter transferred by the companion star: plasma is either accreted or ejected depending on the balance...
Dr
Mikhail Beznogov
(Instituto de Astronomía, Universidad Nacional Autónoma de México)
A neo-neutron star is the next step in a neutron star evolution after the proto-neutron star phase. It begins $30-60$ seconds after the birth of the neutron star when neutrinos are free to escape and the crust of the neutron star is forming. This phase lasts about
$10^4$ seconds until the star "forgets" its initial conditions. Super-Eddington luminosities may still be present for some time....
Dr
Cristobal Espinoza
(Universidad de Santiago de Chile), Mr
Jose Rafael Fuentes
(McGill University)
Glitches are spin-up events that punctuate the smooth rotation of pulsars.
We analyze the glitch sizes $\Delta\nu$ and the times between consecutive events of the seven pulsars with more than 10 detected glitches.
The distributions of glitch sizes of the individual pulsars are different between them (and none of them resembles the global distribution of all known glitches). In particular,...
Mr
Guillaume Voisin
(Jodrell Bank Centre for Astrophysics, The University of Manchester)
Spider pulsars are composed of a millisecond pulsar (MSP) and a low-mass companion, forming the so-called black widows (companion mass Mc < 0.1Msol) and redbacks (Mc>0.1Msol). As MSPs these pulsars are privileged targets for precision timing and possibly timing arrays, but the complex interaction with their companion is still poorly understood and renders their behaviour virtually...
Andreas Schmitt
(University of Southampton)
I will give a review of transport properties of matter inside neutron stars and point out their significance for astrophysical observables. This includes various phases of the star, from the outer layers to the densest possible phases, such as deconfined quark matter. I will mostly focus on general methods and principles, but also discuss specific open questions for future research.
Dr
Guillermo Rodriguez
(National Institute of Astrophysics - Astronomical Observatory of Rome)
The discovery of Ultraluminous X-ray Sources (ULXs) showing fast and rapidly evolving pulsations (PULXs) unambiguously associated
these sources to neutron stars (NSs) exceeding up to more than 500 times their Eddington Luminosity . These discoveries challenge our
understanding of accretion physics and pose a key question about the nature of the ULXs as a class, thought to represent the...
Prof.
Nicolas Chamel
(Université Libre de Bruxelles)
Formed in the aftermath of gravitational core-collapse supernova explosions, neutron stars are the most compact observed stars. Their average density exceeds than that found inside the heaviest atomic nuclei. Neutron stars are also endowed with the strongest magnetic fields known, which can reach millions of billions times that of the Earth. According to our current understanding, a neutron...
Prof.
Veronica Dexheimer
(Kent State University)
Neutron-star mergers can help us understanding what kind of matter exists in the core of compact stars, in addition to new states of matter generated during the events themselves. More specifically, gravitational waves from neutron-star mergers can tell us if quarks can exist in a deconfined way in our universe. Our results include possible signals for a strong deconfinement phase transition...
