Superposition de la distribution d’énergie spectrale de WD 2226-210 sur une image de la nébuleuse Helix du télescope spatial Hubble. Le tracé combine la spectroscopie Spitzer photométrique, infrarouge, millimétrique et infrarouge moyen et les limites supérieures de WISE, Spitzer, SOFIA, Herschel et ALMA. Les modèles de la photosphère (solide) et de l’excès infrarouge de la naine blanche montrent un bon ajustement aux détections de données (cercles) et aux limites supérieures (triangles). Nébuleuse de l’hélice. Crédit : NOIRLab ; Crédit SED : J.P. Marshall.
Une fois qu’une étoile a évolué au-delà de la séquence principale – la plus longue étape de l’évolution stellaire, au cours de laquelle le rayonnement de la fusion nucléaire au cœur de l’étoile est équilibré par la gravité – le sort de tout système planétaire est probablement un mystère. Les astronomes ne savent généralement pas ce qui arrive aux planètes après ce point, ou si elles peuvent survivre.
Dans une recherche récemment publiée dans Le Journal Astronomiqueles chercheurs ont utilisé de nouvelles données de l’Observatoire stratosphérique pour l’astronomie infrarouge ([{ » attribute= » »>SOFIA) and the Atacama Large Millimeter/submillimeter Array (ALMA), as well as archival data from the Spitzer Space Telescope and the Herschel Space Observatory, to study the Helix Nebula. These observations provide one potential explanation for the fate of these planetary remains.
A Process of Elimination, and a Disruptive Origin
The Helix Nebula is an old planetary nebula – expanding, glowing gas ejected from its host star after its main-sequence life ended. The nebula has a very young white dwarf at its center, but this central white dwarf is peculiar. It emits more infrared radiation than expected. To answer the question of where this excess emission comes from, the astronomers first determined where it could not have come from.
Collisions between planetesimals – small, solid objects formed out of cosmic dust left over from the creation of a planetary system around a star – can produce this type of excess emission, but SOFIA and ALMA failed to see the large dust grains required for such objects to exist, ruling out one option. The astronomers also didn’t find any of the carbon monoxide or silicon monoxide molecules characteristic of the gas disks that can surround evolving post-main-sequence stellar systems that precede objects like the Helix Nebula, excluding another potential explanation.
Different strands of evidence place strict constraints on the size, structure, and orbit of the source of the emission, and eventually come together to identify the same culprit: dust – from full-fledged planets destroyed during the nebula’s formation – returning toward its inner regions.
“In piecing together the size and shape of the excess emission, and what those properties infer regarding the dust grains in the white dwarf environment, we conclude that a disrupted planetary system is the best solution to the question of how the Helix Nebula’s infrared excess was created and maintained,” said Jonathan Marshall, the lead author on the paper and a researcher at Academia Sinica in Taiwan.
Once they realized the remnants of a former planetary system are at the origin of the infrared emission, they calculated how many grains need to be returning to the Helix Nebula’s center to account for the emission: about 500 million over the 100,000-year lifetime of the planetary nebula, conservatively.
SOFIA’s Role
SOFIA’s capabilities fell right into a gap between the previous Spitzer and Herschel observations, allowing the group to understand the shape and brightness of the dust, and improving the resolution of how far it spreads out.
“This gap lay around where we expected the dust emission to peak,” Marshall said. “Pinning down the shape of the dust emission is vital to constraining the properties of the dust grains that produce that emission, so the SOFIA observation helped refine our understanding.”
Though the researchers are not planning any follow-up observations of the Helix Nebula in particular, this study is a piece in a larger effort to use observations to understand what happens to planetary systems once their star evolves past the main sequence. The group hopes to study other late-stage stars using similar techniques.
Reference: “Evidence for the Disruption of a Planetary System During the Formation of the Helix Nebula” by Jonathan P. Marshall, Steve Ertel, Eric Birtcil, Eva Villaver, Francisca Kemper, Henri Boffin, Peter Scicluna and Devika Kamath, 19 December 2022, The Astronomical Journal.
DOI: 10.3847/1538-3881/ac9d90
SOFIA was a joint project of NASA and the German Space Agency at DLR. DLR provided the telescope, scheduled aircraft maintenance, and other support for the mission. NASA’s Ames Research Center in California’s Silicon Valley managed the SOFIA program, science, and mission operations in cooperation with the Universities Space Research Association, headquartered in Columbia, Maryland, and the German SOFIA Institute at the University of Stuttgart. The aircraft was maintained and operated by NASA’s Armstrong Flight Research Center Building 703, in Palmdale, California. SOFIA achieved full operational capability in 2014 and concluded its final science flight on September 29, 2022.
