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

The formation time, masses, and location of planets are strongly impacted bythe physical mechanisms that disperse protoplanetary disks and the timescaleover which protoplanetary material is cleared out. Accretion of matter onto thecentral star, protostellar winds/jets, magnetic disk winds, andphotoevaporative winds operate concurrently. Hence, disentangling theirrelative contribution to disk dispersal requires identifying diagnostics thattrace different star-disk environments. Here, we analyze the low velocitycomponent (LVC) of the Oxygen optical forbidden lines, which is found to beblueshifted by a few km/s with respect to the stellar velocity. We find thatthe [OI] LVC profiles are different from those of [NeII] at 12.81\mu m and COat 4.7\mu m lines pointing to different origins for these gas lines. We reporta correlation between the luminosity of the [OI] LVC and the accretionluminosity Lacc. We do not find any correlation with the X-ray luminosity,while we find that the higher is the stellar FUV luminosity, the higher is theluminosity of the [OI] LVC. In addition, we show that the [OI]6300\AA/5577\AA\ratio is low (ranging between 1 and 8). These findings favor an origin of the[OI] LVC in a region where OH is photodissociated by stellar FUV photons andargue against thermal emission from an X-ray-heated layer. Detailed modeling oftwo spectra with the highest S/N and resolution shows that there are twocomponents within the LVC: a broad, centrally peaked component that can beattributed to gas arising in a warm disk surface in Keplerian rotation (withFWHM between ~40 and ~60 km/s), and a narrow component (with FWHM ~10 km/s andsmall blueshifts of ~2 km/s) that may arise in a cool (<1,000 K) molecularwind.

Understanding the origin of the [OI] low-velocity component from T Tauri stars