Open main menu
Home
Random
Recent changes
Special pages
Community portal
Preferences
About Wikipedia
Disclaimers
Incubator escapee wiki
Search
User menu
Talk
Dark mode
Contributions
Create account
Log in
Editing
Helix Nebula
(section)
Warning:
You are not logged in. Your IP address will be publicly visible if you make any edits. If you
log in
or
create an account
, your edits will be attributed to your username, along with other benefits.
Anti-spam check. Do
not
fill this in!
==Central star== [[File:HelixCentralStarLightCurve.png|thumb|left|A light curve for the Helix Nebula central star, adapted from Iskandarli et al. (2024)<ref name="Iskandarli2024"/>]] The central star of the Helix Nebula is a [[white dwarf]] of spectral type DAO.<ref name="Iskandarli2024"/> It has the designations WD 2226-210, PHL 287, and GJ 9785.<ref name="simbad"/> The star has a radius of {{convert|0.025|solar radius|km}}, a mass of {{Solar mass|0.678}}, a temperature of 120,000 [[Kelvin]] and has an apparent magnitude of 13.5.<ref name="Iskandarli2024"/> A mid-infrared excess suggest a disk with a size of 35 to 150 AU, formed from [[Kuiper belt|Kuiper-belt]] like objects.<ref name="Su2007"/> The size was later revised to be a ring between 30 and 100 AU. The non-detection at longer wavelengths allowed a research team to reject a series of scenarios. The researchers think the mid-IR excess comes from a replenishment of dust particles from thousands of [[exocomets]] at high eccentricities, with an origin from an [[Oort cloud]]-like structure.<ref name="Marshall2023"/> A 2024 study hypothesized that the central star might be orbited by a planet based on periodic variations in its [[light curve]], but it cannot be ruled out that these variations are due to intrinsic stellar variability. Assuming an inclination of 25Β° (aligned with the nebula itself), this hypothetical planet is estimated to have a radius of {{convert|0.021|solar radius|km}}, or about 2.3 times the [[Earth radius|radius of Earth]].<ref name="Iskandarli2024"/> Another study from 2025 found from X-ray observation that the central star may be accreting the remains of a Jupiter-like planet. This would be closer than the planet found via optical variability.<ref name="Estrada-Dorado2025"/> {{OrbitboxPlanet begin | table_ref = <ref name="Iskandarli2024"/><ref name="Estrada-Dorado2025"/><ref name="Marshall2023"/> }} {{OrbitboxPlanet hypothetical | exoplanet = c | mass = 1 | semimajor = 0.004 | period = 0.12 | eccentricity = | inclination = | radius_earth = }} {{OrbitboxPlanet hypothetical | exoplanet = b | mass_earth = | semimajor = 0.034 | period = 2.79 | eccentricity = | inclination = ~25? | radius_earth = ~2.3? }} {{OrbitboxPlanet disk | disk = debris disk | periapsis = 30 | apoapsis = 100 | inclination = <!--Inclination from the plane of the sky, in degrees--> }} {{Orbitbox end}}
Edit summary
(Briefly describe your changes)
By publishing changes, you agree to the
Terms of Use
, and you irrevocably agree to release your contribution under the
CC BY-SA 4.0 License
and the
GFDL
. You agree that a hyperlink or URL is sufficient attribution under the Creative Commons license.
Cancel
Editing help
(opens in new window)