Resolving the FU Ori System with ALMA: Interacting Twin Disks?

FU Orionis objects are low-mass pre-main sequence stars characterized by dramatic outbursts of several magnitudes in brightness. These outbursts are linked to episodic accretion events in which stars gain a significant portion of their mass. The physical processes behind these accretion events are n...

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Veröffentlicht in:arXiv.org 2019-11
Hauptverfasser: Pérez, Sebastián, Hales, Antonio, Liu, Hauyu Baobab, Zhu, Zhaohuan, Casassus, Simon, Williams, Jonathan, Zurlo, Alice, Cuello, Nicolás, Lucas Cieza, Principe, David
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creator Pérez, Sebastián
Hales, Antonio
Liu, Hauyu Baobab
Zhu, Zhaohuan
Casassus, Simon
Williams, Jonathan
Zurlo, Alice
Cuello, Nicolás
Lucas Cieza
Principe, David
description FU Orionis objects are low-mass pre-main sequence stars characterized by dramatic outbursts of several magnitudes in brightness. These outbursts are linked to episodic accretion events in which stars gain a significant portion of their mass. The physical processes behind these accretion events are not yet well understood. The archetypical FU Ori system, FU Orionis, is composed of two young stars with detected gas and dust emission. The continuum emitting regions have not been resolved until now. Here, we present 1.3 mm observations of the FU Ori binary system with ALMA. The disks are resolved at 40 mas resolution. Radiative transfer modeling shows that the emission from FU Ori north (primary) is consistent with a dust disk with a characteristic radius of \(\sim\)11 au. The ratio between major and minor axes shows that the inclination of the disk is \(\sim\)37 deg. FU Ori south is consistent with a dust disk of similar inclination and size. Assuming the binary orbit shares the same inclination angle as the disks, the deprojected distance between north and south components is 0.6'', i.e. \(\sim\)250 au. Maps of \(^{12}\)CO emission show a complex kinematic environment with signatures disk rotation at the location of the northern component, and also (to a lesser extent) for FU Ori south. The revised disk geometry allows us to update FU Ori accretion models (Zhu et al.), yielding a stellar mass and mass accretion rate of FU Ori north of 0.6 M\(_{\odot}\) and 3.8\(\times10^{-5}\) M\(_{\odot}\) yr\(^{-1}\), respectively.
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subjects Accretion disks
Astronomical models
Binary stars
Dust
Emission
Inclination angle
Outbursts
Physics - Astrophysics of Galaxies
Physics - Earth and Planetary Astrophysics
Physics - Solar and Stellar Astrophysics
Pre-main sequence stars
Radiative transfer
Rotating disks
Stellar mass
Stellar mass accretion
title Resolving the FU Ori System with ALMA: Interacting Twin Disks?
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