English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We present space-based thermal infrared observations of the presumablyGeminid-associated asteroids: (3200)Phaethon, 2005 UD and 1999 YC usingWISE/NEOWISE. The images were taken at the four wavelength bands3.4$\mu$m(W1),4.6$\mu$m(W2),12$\mu$m(W3),and 22$\mu$m(W4). We find no evidenceof lasting mass-loss in the asteroids over the decadal multi-epoch datasets. Weset an upper limit to the mass-loss rate in dust of Q<2kg s$^{-1}$ for Phaethonand <0.1kg s$^{-1}$ for both 2005 UD and 1999 YC, respectively, with littledependency over the observed heliocentric distances of R=1.0$-$2.3au. ForPhaethon, even if the maximum mass-loss was sustained over the 1000(s)yrdynamical age of the Geminid stream, it is more than two orders of magnitudetoo small to supply the reported stream mass (1e13$-$14kg). ThePhaethon-associated dust trail (Geminid stream) is not detected at R=2.3au,corresponding an upper limit on the optical depth of $\tau$<7e-9. Additionally,no co-moving asteroids with radii r<650m were found. The DESTINY+ dust analyzerwould be capable of detecting several of the 10$\mu$m-sized interplanetary dustparticles when at far distances(>50,000km) from Phaethon. From 2005 UD, if themass-loss rate lasted over the 10,000yr dynamical age of the Daytime Sextantidmeteoroid stream, the mass of the stream would be ~1e10kg. The 1999 YC imagesshowed neither the related dust trail ($\tau$<2e-8) nor co-moving objects withradii r<170m at R=1.6au. Estimated physical parameters from these limits do notexplain the production mechanism of the Geminid meteoroid stream. Lastly, toexplore the origin of the Geminids, we discuss the implications for our data inrelation to the possibly sodium (Na)-driven perihelion activity of Phaethon.

WISE/NEOWISE Multi-Epoch Imaging of the Potentially Geminid-related Asteroids: (3200) Phaethon, 2005 UD and 1999 YC