Millisecond Magnetars

Dall’Osso, S.; Stella, L.

doi:10.1007/978-3-030-85198-9_8

Cited by 12 publications

(5 citation statements)

References 200 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Actually, the rate of SLSNe is estimated to be orders of magnitude lower than the magnetar birth rate (Quimby et al 2013), and indeed represents an issue for any progenitor model, likely pointing to the existence of additional conditions-besides a powerful central engine-to be met in order for an SLSN to occur. Some of these conditions were already discussed (e.g., Metzger et al 2015;Kasen et al 2016); we add here, and discuss further below, that a dominant GW spindown in the early hours after a magnetar birth may provide an additional, straightforward interpretation for this rate mismatch (see, e.g., Dall'Osso & Stella 2007Stella , 2022Dall'Osso et al 2009, 2018.…”

Section: Expected Event Rate and Multimessenger Implicationsmentioning

confidence: 71%

UV Signatures of Magnetar Formation and Their Crucial Role for GW Detection

Menon,

Guetta,

Dall’Osso

2023

ApJ

View full text Add to dashboard Cite

The emission from shock breakouts (SBOs) represents the earliest electromagnetic (EM) signal emitted by cataclysmic events involving the formation or the merger of neutron stars (NSs). As such, SBOs carry unique information on the structure of their progenitors and on the explosion energy. The characteristic SBO emission is expected in the UV range, and its detection is one of the key targets of the ULTRASAT satellite. Among SBO sources, we focus on a specific class involving the formation of fast-spinning magnetars in the core-collapse of massive stars. Fast-spinning magnetars are expected to produce a specific signature in the early UV supernova light curve, powered by the extra spin energy quickly released by the NS. Moreover, they are considered as optimal candidates for the emission of long-transient gravitational wave (GW) signals, the detection of which requires early EM triggers to boost the sensitivity of dedicated GW search pipelines. We calculate early supernova UV light curves in the presence of a magnetar central engine, as a function of the explosion energy, ejecta mass, and magnetar parameters. We then estimate the ULTRASAT detection horizon (z < 0.15) as a function of the same physical parameters, and the overall expected detection rate, finding that magnetar-powered SBOs may represent up to 1/5 of the total events detected by ULTRASAT. Moreover, at the expected sensitivity of the LIGO/Virgo/Kagra O5 science run, one such event occurring within 5 Mpc will provide an ideal trigger for a GW long-transient search. Future GW detectors like the Einstein Telescope will push the horizon for joint EM-GW detections to 35–40 Mpc.

show abstract

Section: Expected Event Rate and Multimessenger Implicationsmentioning

confidence: 71%

UV Signatures of Magnetar Formation and Their Crucial Role for GW Detection

Menon,

Guetta,

Dall’Osso

2023

ApJ

View full text Add to dashboard Cite

show abstract

“…If they result in a neutron star: high frequency normal modes are expected to be excited, related to their interior composition, and produce GWs. Long transient GWs produced by newborn magnetars are also expected, up to a ∼1 per year rate at distances within 30-40 Mpc: the observation of these signals would give us important information on the initial life of magnetars [6,34]. Last, the observation of quasi-normal modes on post-merger BHs will allow us to test near-horizon effects, such as evidences for exotic compact objects [35] and signals from quantum gravity [36].…”

Section: Science Case For Detector Sensitivity Improvements Below 10 Hzmentioning

confidence: 98%

Research Facilities for Europe’s Next Generation Gravitational-Wave Detector Einstein Telescope

et al. 2022

View full text Add to dashboard Cite

The Einstein Telescope is Europe’s next generation gravitational-wave detector. To develop all necessary technology, four research facilities have emerged across Europe: The Amaldi Research Center (ARC) in Rome (Italy), ETpathfinder in Maastricht (The Netherlands), SarGrav in the Sos Enattos mines on Sardinia (Italy) and E-TEST in Liége (Belgium) and its surroundings. The ARC pursues the investigation of a large cryostat, equipped with dedicated low-vibration cooling lines, to test full-scale cryogenic payloads. The installation will be gradual and interlaced with the payload development. ETpathfinder aims to provide a low-noise facility that allows the testing of full interferometer configurations and the interplay of their subsystems in an ET-like environment. ETpathfinder will focus amongst others on cryogenic technologies, silicon mirrors, lasers and optics at 1550 and 2090 nm and advanced quantum noise reduction schemes. The SarGrav laboratory has a surface lab and an underground operation. On the surface, the Archimedes experiment investigates the interaction of vacuum fluctuations with gravity and is developing (tilt) sensor technology for the Einstein Telescope. In an underground laboratory, seismic characterisation campaigns are undertaken for the Sardinian site characterisation. Lastly, the Einstein Telecope Euregio meuse-rhine Site & Technology (E-TEST) is a single cryogenic suspension of an ET-sized silicon mirror. Additionally, E-TEST investigates the Belgian–Dutch–German border region that is the other candidate site for Einstein Telescope using boreholes and seismic arrays and hydrogeological characterisation. In this article, we describe the Einstein Telescope, the low-frequency part of its science case and the four research facilities.

show abstract

“…Actually, other sources of CW-like signals have been investigated. In particular, transient CW signals (tCW) have been considered, such as those expected to be emitted by a newborn magnetar, in the early stages of its evolution [433][434][435][436]. In this case, the frequency secular variation is caused by a combination of the electromagnetic emission, due to the JCAP07(2023)068 super-strong magnetic field, and the gravitational-wave emission, due to the strong asymmetry induced by the electromagnetic field itself.…”

Section: Continuous Wavesmentioning

confidence: 99%

Science with the Einstein Telescope: a comparison of different designs

Branchesi¹,

Maggiore²,

Alonso³

et al. 2023

J. Cosmol. Astropart. Phys.

142

View full text Add to dashboard Cite

The Einstein Telescope (ET), the European project for a third-generation gravitational-wave detector, has a reference configuration based on a triangular shape consisting of three nested detectors with 10 km arms, where each detector has a 'xylophone' configuration made of an interferometer tuned toward high frequencies, and an interferometer tuned toward low frequencies and working at cryogenic temperature. Here, we examine the scientific perspectives under possible variations of this reference design. We perform a detailed evaluation of the science case for a single triangular geometry observatory, and we compare it with the results obtained for a network of two L-shaped detectors (either parallel or misaligned) located in Europe, considering different choices of arm-length for both the triangle and the 2L geometries. We also study how the science output changes in the absence of the low-frequency instrument, both for the triangle and the 2L configurations. We examine a broad class of simple 'metrics' that quantify the science output, related to compact binary coalescences, multi-messenger astronomy and stochastic backgrounds, and we then examine the impact of different detector designs on a more specific set of scientific objectives.

show abstract

Millisecond Magnetars

Cited by 12 publications

References 200 publications

UV Signatures of Magnetar Formation and Their Crucial Role for GW Detection

UV Signatures of Magnetar Formation and Their Crucial Role for GW Detection

Research Facilities for Europe’s Next Generation Gravitational-Wave Detector Einstein Telescope

Science with the Einstein Telescope: a comparison of different designs

Contact Info

Product

Resources

About