The 18 May 2024 Iberian superbolide from a sunskirting orbit: USG space sensors and ground-based independent observations

TL;DR

This study analyzes the 2024 Iberian superbolide using space sensors and ground observations, revealing its origin, physical properties, and orbital characteristics, and providing insights into near-Sun object disruption mechanisms.

Contribution

It combines satellite and ground data to accurately model the meteoroid's atmospheric flight and origin, offering new insights into the physical nature and source region of sunskirting objects.

Findings

Reconciled satellite data with a dynamic atmospheric model.

Identified the meteoroid as a polymict carbonaceous chondrite or thermally processed C-type asteroid.

Suggested origin from the Jupiter-Family Comet region.

Abstract

On 18 May 2024, a superbolide traversed the western part of the Iberian Peninsula, culminating its flight over the Atlantic Ocean and generating significant media attention. This event was caused by a weak carbonaceous meteoroid of 1 m, entering the atmosphere at 40.4 km$\,$s$^{-1}$ with an average slope of 8.5$^\circ$. The luminous phase started at 133 km and ended at an altitude of 54 km. The meteoroid's heliocentric orbit had an inclination of 16.4$^\circ$, a high eccentricity of 0.952, a semi-major axis of 2.4 au, and a short perihelion distance of 0.12 au. The superbolide was recorded by multiple ground-based stations of the Spanish Meteor Network (SPMN) and the European Space Agency (ESA), as well as by the U.S. Government (USG) sensors from space. Due to the absence of observable deceleration, we successfully reconciled satellite radiometric data with a purely dynamic atmospheric flight model, constraining the meteoroid's mass and coherently fitting its velocity profile. Our analysis shows a good agreement with the radiant and velocity data reported by the Center for Near-Earth Object Studies (CNEOS), with a deviation of 0.56$^\circ$ and 0.1 km$\,$s$^{-1}$, respectively. The presence of detached fragments in the lower part of the luminous trajectory suggests that the meteoroid was a polymict carbonaceous chondrite, containing higher-strength macroscopic particles in its interior due to collisional gardening, or a thermally processed C-type asteroid. The orbital elements indicate that the most likely source is the Jupiter-Family Comet (JFC) region, aligning with the SOHO comet family, as its sunskirting orbit is decoupled from Jupiter. This event provides important information to characterize the disruption mechanism of near-Sun objects.