The Structure of the {\beta} Leonis Debris Disk

TL;DR

This study combines multiple observational techniques across a broad wavelength range to analyze the complex debris disk structure around {eta} Leo, revealing multiple dust components and a lack of a typical outer belt.

Contribution

It provides a detailed multi-scale analysis of {eta} Leo's debris disk, highlighting its unique structure compared to similar stars.

Findings

Inner dust ring from 2 to 3 AU with ~600 K temperature

Extended dust zone from ~5 to 55 AU with ~120 K temperature

Absence of a prominent outer belt near 100 AU

Abstract

We combine nulling interferometry at 10 {\mu}m using the MMT and Keck Telescopes with spectroscopy, imaging, and photometry from 3 to 100 {\mu}m using Spitzer to study the debris disk around {\beta} Leo over a broad range of spatial scales, corresponding to radii of 0.1 to ~100 AU. We have also measured the close binary star o Leo with both Keck and MMT interferometers to verify our procedures with these instruments. The {\beta} Leo debris system has a complex structure: 1.) relatively little material within 1 AU; 2.) an inner component with a color temperature of ~600 K, fitted by a dusty ring from about 2 to 3 AU; and 3.) a second component with a color temperature of ~120 K fitted by a broad dusty emission zone extending from about ~5 AU to ~55 AU. Unlike many other A-type stars with debris disks, {\beta} Leo lacks a dominant outer belt near 100 AU.