arXiv subjects

Carolin N. Kimmig

Publications and source records attributed to Carolin N. Kimmig.

3 recordsLinked to original sources

arXiv2026

The Structure and Kinematics of Three Class 0 Protostellar Jets from JWST

We present observations of jets within 2000 au of three deeply embedded protostars using 2.9-27 micron observations with JWST. These observations show the morphologies and kinematics of the collimated jets from three protostars, the low-mass Class 0 protostars B335 and HOPS 153, and the intermediate-mass protostar HOPS 370. These jets are traced by shock-ionized fine-structure line emission observed with the JWST NIRSpec and MIRI IFUs. We find that [Fe II] emission traces the full extent of the inner 1000 to 2000 au of the jets, depending on distance to the protostar, while other ions mostly trace isolated shocked knots. The jets show evidence of wiggling motion in the plane of the sky as well as asymmetries between blue and red-shifted lobes. The widths of the jets increase non-monotonically with distance from the central protostar, with opening angles ranging from 2.1 degrees to < 10.1 degrees for the three protostars in the sample. The jets have total velocities ranging from 147 to 184 km/s after correcting for disk inclination. For B335, an 8-month gap between NIRSpec and MIRI MRS observations enabled measurement of the tangential velocity of a shocked knot; in combination with the radial velocity, this shows that the jet has a different inclination than the outflow cavity. We find multiple knots before and during a recent outburst in B335, although the knots were more frequent during the burst. The asymmetries between blue- and red-shifted lobes strongly suggest complex interactions between the circumstellar disks and magnetic fields.

astro-ph.SR↗

arXiv2025

exoALMA. XVIII. Interpreting large scale kinematic structures as moderate warping

The exoALMA program gave an unprecedented view of the complex kinematics of protoplanetary disks, revealing diverse structures that remain poorly understood. We show that moderate disk warps ($\sim 0.5-2^\circ$) can naturally explain many of the observed large-scale velocity features with azimuthal wavenumber $m = 1$. Using a simple model, we interpret line-of-sight velocity variations as changes in the projected Keplerian rotation caused by warping of the disk. While not a unique explanation, this interpretation aligns with growing observational evidence that warps are common. We demonstrate that such warps can also produce spiral structures in scattered light and CO brightness temperature, with $\sim 10$ K variations in MWC 758. Within the exoALMA sample, warp properties correlate with stellar accretion rates, suggesting a link between the inner disc and outer disc kinematics. If warps cause large-scale kinematic structure, this has far reaching implications for turbulence, angular momentum transport, and planet formation.

astro-ph.EP↗

arXiv2025

Asymmetric Signatures of Warps in Edge-on Disks

Protoplanetary disks observed edge-on commonly show asymmetries that can be caused by shadows cast from a warp. With the growing amount of these observations, methods to constrain warp parameters are urgently needed. In this work, we investigate observational signatures of warps in edge-on disks with the aim to find limits on the observability of warps. We perform radiative transfer simulations in scattered light (near-/mid-infrared) of edge-on disks containing warps of different amplitudes and varying sizes of the misaligned inner region. We analyze the effect of these parameters at 0.8 micron, but also compare models for specific parameters at wavelengths up to 21 micron. In all models, we quantify the apparent asymmetry. We find that under optimal conditions, an asymmetry due to slight warps can be visible. The visibility depends on the viewing angle, as warped disks are not axisymmetric. For optimal azimuthal orientation, misalignments between inner and outer disk regimes as low as 2° can lead to significant asymmetries. On the other hand, we find that larger misalignments of about 10° are needed in order to observe a change in the brightest nebula as a function of wavelength, which is observed in a few protoplanetary disks. In order to link our results to observations, we investigate potential misalignments between the inner and outer disk of edge-on systems showing asymmetries. We compare the jet geometry, which traces the inner region of the disk, to the outer disk orientation and find that a misalignment of a few degrees could be present, such that warped disks could explain the apparent lateral asymmetries. There are many factors that can influence the appearance of the shadows and asymmetries in warped disks. Although it is still challenging to infer exact warp parameters from observations, this work presents a promising step toward better constraints.

astro-ph.SR↗