A Young White Dwarf Companion to Pulsar B1620-26: Evidence for Early Planet Formation

@article{Sigurdsson2003AYW,
  title={A Young White Dwarf Companion to Pulsar B1620-26: Evidence for Early Planet Formation},
  author={Steinn Sigurdsson and Harvey B. Richer and Brad Hansen and Ingrid H. Stairs and Stephen Erik Thorsett},
  journal={Science},
  year={2003},
  volume={301},
  pages={193 - 196}
}
The pulsar B1620-26 has two companions, one of stellar mass and one of planetary mass. We detected the stellar companion with the use of Hubble Space Telescope observations. The color and magnitude of the stellar companion indicate that it is an undermassive white dwarf (0.34 ± 0.04 solar mass) of age 480 × 106 ± 140 × 106 years. This places a constraint on the recent history of this triple system and supports a scenario in which the current configuration arose through a dynamical exchange… 
A Jovian analogue orbiting a white dwarf star.
TLDR
The non-detection of a main-sequence lens star in the microlensing event MOA-2010-BLG-477Lb12 using near-infrared observations from the Keck Observatory is reported, which is evidence that planets around white dwarfs can survive the giant and asymptotic giant phases of their host's evolution, and supports the prediction that more than half ofwhite dwarfs have Jovian planetary companions.
The Pulsar/White Dwarf/Planet System in M4: Improved Astrometry
A young and undermassive white dwarf has been identified as the possible companion to the millisecond pulsar PSR B1620-26 in M4. This association is important since it then helps constrain the mass
A search for cold dust around neutron stars
We present observations of nine radio pulsars using the Heinrich-Hertz-Telescope at λ 0.87 mm and the IRAM 30-m telescope at λ 1.2 mm in search for a cold dust around these sources. Five of the
The Core Accretion Model Predicts Few Jovian-Mass Planets Orbiting Red Dwarfs
The favored theoretical explanation for giant planet formation—in both our solar system and others—is the core accretion model (although it still has some serious difficulties). In this scenario,
The planet in M4: implications for planet formation in globular clusters
We consider the formation and evolution of the planetary system PSR B1620‐26 in the globular cluster M4. We propose that as M4 is a very low-metallicity environment the standard model of planet
LIMITS ON PLANET FORMATION AROUND YOUNG PULSARS AND IMPLICATIONS FOR SUPERNOVA FALLBACK DISKS
We have searched a sample of 151 young, energetic pulsars for periodic variation in pulse time-of-arrival arising from the influence of planetary companions. We are sensitive to objects with masses
The Helium White Dwarf Orbiting the Millisecond Pulsar in the Halo of the Globular Cluster NGC 6752
We have used deep high-resolution multiband images taken at the ESO Very Large Telescope to identify the optical binary companion to the millisecond pulsar (PSR J1911-5958A) located in the halo of
Planetary magnetosphere evolution around post-main-sequence stars
Accompanying the mounting detections of planets orbiting white dwarfs and giant stars are questions about their physical history and evolution, particularly regarding detectability of their
M dwarfs: planet formation and long term evolution
The first part of this paper discusses how planet formation proceeds in the disks orbiting M dwarf stars. These environments are different from those associated with solar-type stars in several ways:
Neutron Star Planets: Atmospheric processes and habitability
Of the roughly 3000 neutron stars known, only a handful have sub-stellar companions. The most famous of these are the low-mass planets around the millisecond pulsar B1257+12. New evidence indicates
...
...

References

SHOWING 1-10 OF 26 REFERENCES
Helium Core White Dwarfs in Globular Clusters
We examine the theoretical implications of a population of low-mass helium core white dwarfs in globular clusters. In particular, we focus on the observed population in the core of NGC 6397, where
Theoretical Implications of the PSR B1620–26 Triple System and Its Planet
We present a new theoretical analysis of the PSR B1620-26 triple system in the globular cluster M4, based on the latest radio pulsar timing data, which now include measurements of five time
A second companion of the millisecond pulsar 1620 – 26
MILLISECOND pulsars are usually found in binary systems. This is in keeping with the generally accepted model for the formation of such pulsars14 in which an old neutron star is spun up to high
Orbital migration of the planetary companion of 51 Pegasi to its present location
THE recent discovery1 and confirmation2 of a possible planetary companion orbiting the solar-type star 51 Pegasi represent a breakthrough in the search for extrasolar planetary systems. Analysis of
White Dwarfs in Globular Clusters: Hubble Space Telescope Observations of M4
Using WFPC2 on the Hubble Space Telescope, we have isolated a sample of 258 white dwarfs (WDs) in the Galactic globular cluster M4. Fields at three radial distances from the cluster center were
The Triple Pulsar System PSR B1620–26 in M4
The millisecond pulsar PSR B1620-26, in the globular cluster M4, has a white dwarf companion in a half-year orbit. Anomalously large variations in the pulsar's apparent spin-down rate have suggested
Discovery of a binary millisecond pulsar in the globular cluster M4
We report the discovery of an 11-ms pulsar, PSR1620–26, in the closest globular cluster, M4 (NGC6121). It is the fifth millisecond pulsar to be found, and the second in a globular cluster. Unlike the
The Temperature and Cooling Age of the White Dwarf Companion to the Millisecond Pulsar PSR B1855+09
TLDR
On Keck and Hubble Space Telescope observations of the binary millisecond pulsar PSR B1855+09, it is inferred that helium white dwarfs form with thick hydrogen layers, with mass greater, similar3x10-3 M middle dot in circle, which leads to significant additional heating.
The Luminosity Function of the Globular Cluster NGC 6397 near the Limit of Hydrogen Burning
Second-epoch Hubble Space Telescope observations of NGC 6397 have led to the measurement of proper motions accurate enough to separate the faintest cluster stars from the field, thus extending the
Migrating planets
TLDR
A planet orbiting in a disk of planetesimals can experience an instability in which it migrates to smaller orbital radii, which may explain the presence of Jupiter-mass objects in small orbits around nearby stars.
...
...