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EPSILON ERIDANI’S PLANETARY DEBRIS DISK: STRUCTURE AND . . . Spitzer and Caltech Submillimeter Observatory images and spectrophotometry of Eridani at wavelengths from 3 5 to 350 μm reveal new details of its bright debris disk The 350 μm map confirms the presence of a ring at r = 11 –28 (35–90 AU), observed previously at longer sub-mm wavelengths
arXiv:1606. 08553v1 [astro-ph. SR] 28 Jun 2016 ABSTRACT We present simultaneous ground-based radial velocity (RV) measurements and space-based photo- metric measurements of the young and active K dwarf Epsilon Eridani These measurements provide a data set for exploring methods of identifying and ultimately distinguishing stellar photospheric ve- locities from Keplerian motion
DETECTING A PLANET BY ROTATION OF STRUCTURE IN THE EPSILON . . . Introduction: We present submillimetre images of the epsilon Eridani debris disk, made between 1997 and 2002 using the SCUBA camera at 450 and 850 microns [1,2] The thermal emission of dust particles traces debris generated by collisions amongst a belt of comets, situated between 40 and 90 AU from the star
Epsilon Eridani Debris Disk Using ALMA to Constrain Epsilon Eridani (K2) is the closest Sun-like star (at 3 22 pc) with a planetary system hosting both an inner and outer debris disk along with a roughly Jupiter-mass planet at ~3 5 au (Epsilon Eridani b)
EPSILON ERIDANI’S PLANETARY DEBRIS DISK: STRUCTURE AND . . . Spitzer and Caltech Submillimeter Observatory images and spectrophotometry of Eridani at wavelengths from 3 5 to 350 μm reveal new details of its bright debris disk The 350 μm map confirms the presence of a ring at r 11 –28 (35–90 AU), observed previously at longer sub-mm wavelengths
MODELING THE GLOBAL OSCILLATIONS OF EPSILON ERIDANI David R . . . strength of the chromospehric emission is also only a staistical age indicator Epsilon Eri is unarguably an active star: it has strong Ca II H and Κ emission (Noyes et al 1984), strong UV emissions (Kelch 1978; Linsky et al 1982), and strong X-ray emission (Johnson 1981)
THE EPSILON ERIDANI SYSTEM RESOLVED BY MILLIMETER INTERFEROMETRY We present observations of ϵ Eridani from the Submillimeter Array (SMA) at 1 3mm and from the Australia Telescope Compact Array at 7mm that reach an angular resolution of ∼4″ (13AU) These first millimeter interferometer observations of ϵ Eridani, which hosts the closest debris disk to the Sun, reveal two distinct emission