copy and paste this google map to your website or blog!
Press copy button and paste into your blog or website.
(Please switch to 'HTML' mode when posting into your blog. Examples: WordPress Example, Blogger Example)
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