arXiv subjects

S. Bloot

Publications and source records attributed to S. Bloot.

4 recordsLinked to original sources

arXiv2026

Radio emission from star-planet interactions

Stars interact with their exoplanets though gravity, radiation, plasma and magnetic fields. Stellar plasma and magnetic fields impose electrodynamic effects on exoplanet atmospheres and interiors that include heating, aurorae and atmospheric mass loss. The planets in turn can excite Alfv\'enic disturbances that are dissipated on the star leading to chromospheric heating and flares. This interaction, broadly called magnetic star-planet interaction (M-SPI), can also generate radio signatures both from the star and the exoplanet. The radio emission encodes information on the dynamics/energetics of the interaction, the magnetic field strength and topology of the emitter and the orbital/rotational geometry of the system -- information that is difficult or in some cases implausible to obtain by other means. Yet we do not have a conclusive detection of M-SPI in the radio band primarily due to sensitivity limitations and scarce observing time spent monitoring promising targets. Here we describe the scientific motivation to study M-SPI in exoplanetary systems, to get progress in understanding its predicted signal strength and phenomenology. We argue that the SKA telescopes can make a transformative contribution to exoplanet science by detecting M-SPI in the radio band but this will require substantial observing time -- similar to that afforded to successful optical-band searches for M-SPI signatures.

astro-ph.EP↗

arXiv2025

Radio Burst from a Stellar Coronal Mass Ejection

Coronal mass ejections (CMEs) are massive expulsions of magnetised plasma from a star, and are the largest contributors to space weather in the Solar System. CMEs are theorized to play a key role in planetary atmospheric erosion, especially for planets that are close to their host star. However, such a conclusion remains controversial as there has not been an unambiguous detection of a CME from a star outside of our Sun. Previous stellar CME studies have only inferred the presence of a CME through the detection of other types of stellar eruptive events. A signature of a fast CME is a Type II radio burst, which is emitted from the shock wave produced as the CME travels through the stellar corona into interplanetary space. Here we report an analogue to a Type II burst from the early M dwarf StKM 1-1262. The burst exhibits identical frequency, time, and polarisation properties to fundamental plasma emission from a solar Type II burst. We demonstrate the rate of such events with similar radio luminosity from M dwarfs are 0.84$^{+1.94}_{-0.69} \times$10$^{-3}$ per day per star. Our detection implies that we are no longer restricted to extrapolating the solar CME kinematics and rates to other stars, allowing us to establish the first observational limits on the impact of CMEs on exoplanets.

astro-ph.SR↗

arXiv2022

V-LoTSS: The Circularly-Polarised LOFAR Two-metre Sky Survey

We present the detection of 68 sources from the most sensitive radio survey in circular polarisation conducted to date. We use the second data release of the 144 MHz LOFAR Two-metre Sky Survey to produce circularly-polarised maps with median 140 $\mu$Jy beam$^{-1}$ noise and resolution of 20$''$ for $\approx$27% of the northern sky (5634 deg$^{2}$). The leakage of total intensity into circular polarisation is measured to be $\approx$0.06%, and our survey is complete at flux densities $\geq1$ mJy. A detection is considered reliable when the circularly-polarised fraction exceeds 1%. We find the population of circularly-polarised sources is composed of four distinct classes: stellar systems, pulsars, active galactic nuclei, and sources unidentified in the literature. The stellar systems can be further separated into chromospherically-active stars, M dwarfs, and brown dwarfs. Based on the circularly-polarised fraction and lack of an optical counterpart, we show it is possible to infer whether the unidentified sources are likely unknown pulsars or brown dwarfs. By the completion of this survey of the northern sky, we expect to detect 300$\pm$100 circularly-polarised sources.

astro-ph.GA↗

arXiv2021

Radio modelling of the brightest and most luminous non-thermal colliding-wind binary Apep

Apep is the brightest and most luminous non-thermal colliding-wind binary by over an order of magnitude. It has been suggested from infrared observations that one of the Wolf-Rayet stars in Apep is launching an anisotropic wind. Here we present radio observations of Apep from 0.2 to 20 GHz taken over 33 years. The spectrum reveals an extremely steep turnover in the flux density at low frequencies, where the flux density decreases by two orders of magnitude over only 325 MHz of bandwidth. This exponential decline is best described by free-free absorption, with a turnover frequency at 0.54 $\pm$ 0.01 GHz. Above the turnover, the spectrum is well described by a power-law and a high-frequency cut-off likely caused by inverse-Compton cooling. The lightcurve of Apep shows significant variation over the observing period, with Apep brightening by over 50 mJy in a span of 25 years at 1.4 GHz. Models that assume spherical winds do not replicate all of the structure evident in the radio lightcurve. We derived a model that allows one of the winds in the system to be anisotropic. This anisotropic model recovers most of the structure of the lightcurve and is a significantly better statistical fit to the data than the spherical wind model. We suggest such a result is independent support that one of the Wolf-Rayet stars in Apep is launching an anisotropic wind. If the anisotropic wind model is correct, we predict a ~25% decrease of the 1.4 GHz flux density of Apep over the next five years.

astro-ph.SR↗