ausblenden:
Schlagwörter:
PLANET-FORMING DISKS; WEBB-SPACE-TELESCOPE; LOW-MASS STARS;
PROTOPLANETARY DISKS; T-TAURI; MIDINFRARED INSTRUMENT; ORBITAL MOTION;
DUST EVOLUTION; COOL WATER; INNER DISKAstronomy & Astrophysics; instrumentation: interferometers; instrumentation: spectrographs;
planets and satellites: formation; protoplanetary disks; binaries:
general; stars: pre-main sequence;
Zusammenfassung:
Context. The majority of young stars form in multiple systems, the properties of which can significantly impact the evolution of any circumstellar disks.
Aims. We investigate the physical and chemical properties of the equal-mass, small-separation (similar to 66 milliarcsecond, similar to 9 au) binary system DF Tau. Previous spatially resolved observations indicate that only DF Tau A has a circumstellar disk, while DF Tau B does not, as concluded by a lack of accretion signatures and a near-infrared excess.
Methods. We present JWST-MIRI MRS observations of DF Tau. The MIRI spectrum shows emission from a forest of H2O lines and emission from CO, C2H2, HCN, CO2, and OH. Local thermodynamic equilibrium slab models were used to determine the properties of the gas. The binary system is not spatially or spectrally resolved in the MIRI observations; therefore, we analyzed high spatial and spectral resolution observations from ALMA, VLTI-GRAVITY, and IRTF-iSHELL to aid in the interpretation of the molecular emission observed with JWST.
Results. The 1.3 mm ALMA observations show two equal-brightness sources of compact (R less than or similar to 3 au) continuum emission that are detected at high significance, with separations consistent with astrometry from VLTI-GRAVITY and movement consistent with the known orbital parameters of the system. We interpret this as a robust detection of the disk around DF Tau B, which we suggest may host a small (similar to 1 au) cavity; such a cavity would reconcile all of the observations of this source. In contrast, the disk around DF Tau A is expected to be a full disk, and spatially and spectrally resolved dust and gas emission traced by ground-based infrared observations point to hot, close-in (less than or similar to 0.2 au) material around this star. High-temperature emission (similar to 500-1000 K) from H2O, HCN, and potentially C2H2 in the MIRI data likely originates in the disk around DF Tau A, while a cold H2O component (less than or similar to 200 K) with an extended emitting area is consistent with an origin from both disks.
Conclusions. Given the unique characteristics of this binary pair, complementary observations are critical for constraining the properties of these disks. Despite the very compact outer disk properties, the inner disk composition and the conditions of the DF Tau disks are remarkably similar to those of isolated systems, suggesting that neither the outer disk evolution nor the close binary nature are driving factors in setting the inner disk chemistry in this system. However, constraining the geometry of the disk around DF Tau B, via higher angular resolution ALMA observations for instance, would provide additional insight into the properties of the mid-infrared gas emission observed with MIRI. JWST observations of spatially resolved binaries, at a range of separations, will be important for understanding the impact of binarity on inner disk chemistry more generally.
