Date: January 31, 2024Time: 1:00 pm – 2:00 pm Eastern TimeLocation: WebExhttps://nasaenterprise.webex.com/nasaenterprise/j.php?MTID=m9d2e70c81ad38d00eda138b6aaf57c67
Date: January 31, 2024Time: 1:00 pm – 2:00 pm Eastern TimeLocation: WebExhttps://nasaenterprise.webex.com/nasaenterprise/j.php?MTID=m9d2e70c81ad38d00eda138b6aaf57c67
![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://astrobiology.newspackstaging.com/wp-content/uploads/2025/02/Stellar-Magnetic-Fingerprints.png)
