The planet-forming disk of HD 142527 is known for its azimuthally asymmetric dust trap, shadows, and spiral arms.
HD 142527
![Stokes I (top), polarized intensity (PI) (middle) and polarization fraction (PF) (bottom) at 0.87, 1.3, 2.1 and 2.7 mm wavelengths plotted against right ascension (Δα) and declination (Δδ). Polarization vectors are also shown on the PI and PF images. The Stokes I and PI are converted to the brightness temperature (TB) by assuming the Rayleigh–Jeans approximation. The PF and polarization vectors are plotted where the polarized intensity is detected above the 3σ noise level. Contours on the PI and PF images indicate the brightness temperatures of the Stokes I emission of [0.1, 1, 10, 20] K for 0.87 mm, [0.1, 1, 5, 10, 20] K for 1.3 mm, [0.1, 1, 5, 9] K for 2.1 mm and [0.06, 0.3, 1, 3] K for 2.7 mm. The resolution (beam size) is shown as a small ellipse in the lower left corner of each panel. -- NAOJ](https://i0.wp.com/astrobiology.com/wp-content/uploads/2025/02/Stellar-Magnetic-Fingerprints.png?resize=1200%2C719&ssl=1)
Posted inAstrogeology, Astronomy & Telescopes, Exoplanets, -moons, -comets, Magnetic Fields, Electromagnetism, bioelectricity,, Press Release
Stellar Magnetic Fingerprints And Planetary Formation
For the first time astronomers have succeeded in observing the magnetic field around a young star where planets are thought to be forming. The team was able to use dust […]