activity
20042009
most citedNonthermal Hard X-ray Emission and Iron Kalpha Emission from a Superflare on II Pegasi

105 citations · 371 across the 9 of their papers we have counts for

collaborators
Showing astro-phShow all

9 papers · 1 filter

astro-ph20085 cited

Transient Emissions from Radio-Active Stars: Implications for Wide-Field Radio Surveys

Rachel A. Osten

Variability is a common characteristic of magnetically active stars. Flaring variability is usually interpreted as the observable consequence of transient magnetic reconnection pro…

astro-ph200770 cited

Ultra-high-time Resolution Observations of Radio Bursts on AD Leonis

R. A. Osten, T. S. Bastian

We report observations of a radio burst that occurred on the flare star AD Leonis over a frequency range of 1120-1620 MHz (lambda ~18-27 cm). These observations, made by the 305m t…

astro-ph200753 cited

A Chandra X-ray detection of the L dwarf binary Kelu-1: Simultaneous Chandra and Very Large Array observations

M. Audard, R. A. Osten, A. Brown +4

Magnetic activity in ultracool dwarfs, as measured in X-rays and H, shows a steep decline after spectral type M7-M8. So far, no L dwarf has been detected in X-rays. In contrast,…

astro-ph200646 cited

Discovery of Radio Emission from the Tight M8 Binary: LP 349-25

N. Phan-Bao, R. A. Osten, J. Lim +2

We present radio observations of 8 ultracool dwarfs with a narrow spectral type range (M8-M9.5) using the Very Large Array at 8.5 GHz. Only the tight M8 binary LP 349-25 was detect…

astro-ph2006105 cited

Nonthermal Hard X-ray Emission and Iron Kalpha Emission from a Superflare on II Pegasi

R. A. Osten, S. Drake, J. Tueller +4

We report on an X-ray flare detected on the active binary system II~Pegasi with the Swift telescope. The trigger had a 10-200 keV luminosity of 2.2 erg s-- a…

astro-ph200622 cited

Radio Constraints on Activity in Young Brown Dwarfs

R. A. Osten, R. Jayawardhana

We report on searches for radio emission from three of the nearest known young brown dwarfs using the Very Large Array. We have obtained sensitive upper limits on 3.6cm emission fr…