Lost in space: companions' fatal dance around massive dying stars

Abstract

Discoveries of planet- and stellar remnant-hosting pulsars challenge our understanding as the violent supernova explosion that forms the pulsar presumably destabilizes the system. Type II supernova explosions lead to the formation of eccentric bound systems, free-floating planets, neutron stars, pulsars, and white dwarfs. Analytical and numerical studies of high mass-loss rate systems based on perturbation theory so far have focused mainly on planet-star systems. In this paper, we extend our understanding of the fate of planet-star and binary systems by assuming a homologous envelope expansion model using a plausible ejection velocity ($1000-10000km/s$), envelope- and neutron star masses. The investigation covers secondary masses of 1-10MJup for planetary, and 1-20MSun for stellar companions. We conduct and analyze over 2.5 million simulations assuming different semi-major axes (2.23 - 100au), eccentricities (0-0.8), and true-anomalies (0-2pi) for the companion. In a homologous expansion scenario, we confirm that the most probable outcome of the explosion is the destabilization of the system, while the retention of a bound system requires a highly eccentric primordial orbit. In general, a higher ejecta velocity results in a lower eccentricity orbit independent of secondary mass. The explanation of close-in pulsar planets requires exotic formation scenarios, rather than survival through the type II supernova explosion model. Post-explosion bound star systems gain a peculiar velocity (<100\,km/s), even though the explosion model is symmetric. The applied numerical model allows us to derive velocity components for dissociating systems. The peculiar velocities of free-floating planets and stellar corpses are in the range of 10^-6-275km/s.

arXiv commentAccepted for publication in ApJ (proofread)

References in corpus (48)

• The ATNF Pulsar Catalogue
• Comprehensive analytic formulae for stellar evolution as a function of mass and metallicity
• A statistical study of 233 pulsar proper motions
• Protoplanetary Disks and Their Evolution
• The Stellar IMF from Turbulent Fragmentation
• The death of massive stars - I. Observational constraints on the progenitors of type II-P supernovae
• The Formation of Brown Dwarfs as Ejected Stellar Embryos
• Analytical theory for the initial mass function: CO clumps and prestellar cores
• Unbound or Distant Planetary Mass Population Detected by Gravitational Microlensing
• Planet formation around stars of various masses: The snow line and the frequency of giant planets
• Are There Unstable Planetary Systems Around White Dwarfs?
• The Maximum Mass of a Neutron Star
• A Population of very young Brown Dwarfs and free-floating Planets in Orion
• A Young White Dwarf Companion to Pulsar 1620-26: Evidence for Early Planet Formation
• Type II Supernovae as Standardized Candles
• The Exoplanet Orbit Database II: Updates to exoplanets.org
• Dynamical effects of stellar mass loss on a Kuiper-like belt
• The Great Escape: How Exoplanets and Smaller Bodies Desert Dying Stars
• Physical parameters of the high-mass X-ray binary 4U1700-37
• The Formation of Free-Floating Brown Dwarves and Planetary-Mass Objects by Photo-Erosion of Prestellar Cores
• Transformation of a Star into a Planet in a Millisecond Pulsar Binary
• Planet-Planet Scattering Alone Cannot Explain the Free-Floating Planet Population
• A rich population of free-floating planets in the Upper Scorpius young stellar association
• Brown dwarf disks with ALMA: evidence for truncated dust disks in Ophiuchus
• The fate of fallback matter around newly born compact objects
• Stability and Evolution of Supernova Fallback Disks
• First versus second generation planet formation in post common envelope binary (PCEB) planetary systems
• Candidate free-floating super-Jupiters in the young sigma Orionis open cluster
• Timing Gamma-ray Pulsars with the Fermi Large Area Telescope: Timing Noise and Astrometry
• A Giant Planet Around a Metal-poor Star of Extragalactic Origin
• Planet formation from the ejecta of common envelopes
• On the Number of Comets Around White Dwarf Stars: Orbit Survival During the Late Stages of Stellar Evolution
• WD 1856 b: a close giant planet around a white dwarf that could have survived a common-envelope phase
• A population of transition disks around evolved stars: Fingerprints of planets? Catalog of disks surrounding Galactic post-AGB binaries
• PSR J2322$-$2650 -- A low-luminosity millisecond pulsar with a planetary-mass companion
• Hyperfast pulsars as the remnants of massive stars ejected from young star clusters
• Possible Implications of the Planet Orbiting the Red Horizontal Branch Star HIP 13044
• On the Origin of the Eccentricities of Extrasolar Planets
• Distance of the Hypernova SN 2002ap via the Expanding Photosphere Method
• Tatooine's Future: The Eccentric Response of Kepler's Circumbinary Planets to Common-Envelope Evolution of their Host Stars
• Why are pulsar planets rare?
• Successive common envelope events from multiple planets
• Evidence for multiple origins of fast declining Type II supernovae from spectropolarimetry of SN 2013ej and SN 2017ahn
• A Search for Cold Dust around Neutron Stars
• A wide planetary-mass companion to a young low-mass brown dwarf in Ophiuchus
• On The Existence of Planets Around the Pulsar PSR B0329+54
• Planet formation in post-common-envelope binaries
• Lucky planets: how circum-binary planets survive the supernova in one of the inner-binary components

Cited by in corpus (2)

• Double neutron star formation via consecutive type II supernova explosions
• Life in the dark: Potential urability of moons of rogue planets