Forming misaligned disks through late infall

Michael Küffmeier

C. P. Dullemond, F. Goicovic, S. Reißl, A. Krieger

Marie-Skłodowska-Curie fellow, Carlsberg Reintegration fellow

 Sequence of star, disk & planet formation

Pineda ... Küffmeier et al. 'Protostars and Planets VII'

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Segura-Cox et al. in prep.

Star & disk can be replenished by infall of initially unbound material

Credit: ALMA (ESO/NAOJ/NRAO)

Ginski et al. 2021

Yen et al. 2019

Garufi et al. 2021

Pineda et al. 2020

50 au

BHB1 (Alves et al. 2020), GM Aur (Huang et al. 2021), IRS 63 (Segura-Cox in prep.), AB Aur (Grady et al. 1999 / Fukagawa et al. 2004), M512 Grant et al. 2021, Cacciapuoti in prep.), ...

Per-emb-50

Valdivia-Mena et al. 2022

Streamers: recall A. Gupta's talk

Late infall 

AB Aurigae

HD 100546

Credit: Grady+ 1999, Fukagawa+ 2004

Can (late) infall cause misalignment of inner and outer disk?

Credit: Ardila+ 2007

200 au

HD 142527

Credit: Avenhaus+ 2014

Extended arc-like structures can be induced by late infall

(Dullemond, Küffmeier, Goicovic+ 2019, Küffmeier, Goicovic & Dullemond 2020)

Possibility of "second-generation" disk

Shadows due to misaligned inner and outer disk

Credit: Marino+ 2015

Simulate cloudlet infall onto disk

AREPO, pure hydro

R_{\rm i,d}=50\, \rm au
\Sigma(r) = 170 \left(\frac{\rm g}{\rm cm^{2}}\right) \left( \frac{r}{1 \rm au} \right)^{-3/2}
M_{\rm cloudlet}(R_{\rm cloudlet}) = 0.01 {\rm M}_{\odot} \left( \frac{R_{\rm cloudlet}}{5000 \rm au}\right)^{2.3}
R_{\rm cloudlet} = 887\, \rm au

isothermal gas

vary infalling angle

\alpha = 0^{\circ} (35^{\circ}, 60^{\circ}, 90^{\circ})
b = 1774\, \rm au

vary rotation (prograde, retrograde)

Küffmeier, Dullemond, Reißl, Goicovic 2021

M_{*}=2.5\, \mathrm{M}_{\odot}

Outer disk forms around inner disk

Küffmeier+ 2021

consistent with star formation simulations by Bate '18

Prograde vs. retrograde infall

Retrograde infall causes:

  • counter-rotating inner and outer disk 
  • shrinking of inner disk
  • enhanced accretion
  • larger and deeper gap between disks

see also Vorobyov+ 2016

Küffmeier+ 2021

Streamers and shadows as signs of infall?

Formation of misaligned configuration

Observable as shadows in outer disk

Küffmeier, Dullemond, Reissl & Goicovic 2021

in agreement with Thies+ 2011, Bate 2018

Ginski et al. 2021 (see also Labdon et al. 2023)

300 au

(follow-up study on synthetic signatures currently in prep: Krieger, Küffmeier, Reissl et al.)

Streamers and shadows as signs of infall.

Disk evolution: eccentricity

prograde, 0°

Light to dark: retrograde infall with increasing inclination

  • mild eccentricity in inner disk (up to ~0.1)

inner

outer

  • larger eccentricities in outer disk (0.2 to 0.4)

Infall triggers:

=> test infall scenario in CO channel maps

Küffmeier, Dullemond, Reissl & Goicovic 2021

Inner disk orientation

M_{\rm i, disk}=4 \ M_{\rm cloudlet}
M_{\rm cloudlet} = 1.87 \times 10^{-4} \ \mathrm{M}_{\odot}
M_{\rm i,disk} = 24 M_{\rm cloudlet}
M_{\rm i,disk}=4 \ M_{\rm cloudlet}
M_{\rm i,disk} = 0.4 \ M_{\rm cloudlet}

Küffmeier+ 2021

WIP: Zoom-in self-consistently on late infall

Küffmeier in prep.

Disclaimer:

We are not saying that all shadows are due to misaligned infall!

In some cases shadows have already been well explained by external companions and/or inner planets (e.g.: HD 100453 Gonzalez+ '20/Nealon+ '20 or work by Zhu '19 on planet-induced misalignment)  

Infall mechanism in perspective

But we need to think outside the disk:

significant fraction of final mass might accrete late through inflow (Küffmeier+ 2023, Pelkonen+ 2020)

Pineda et al. 2020; see also [BHB2007] 1 (Alves et al. 2020)

Küffmeier et al. 2019

binaries/fly-bys (see review by Cuello+ 2023 and references therein)

environmental effects (Cathie's talk): photoevaporation (e.g., Haworth+2020), cosmic-rays (e.g., Küffmeier+ 2020), ...

Take-away points

The young outer disk is expected to have higher eccentricity than the old inner disk.

Retrograde infall can cause counter-rotating disks, shrinking of inner disk, formation of gaps (>10 AU) and enhanced accretion.

WIP: zoom-in simulations to self-consistently account for late infall onto star-disk systems 

On average, stars with final masses of more than 1 solar mass accrete >50 % of their mass after 500 kyr

Küffmeier, Jensen & Haugbølle '23

Heterogeneous accretion implies late infall

Observational indication: luminosity bursts

(PPVII review by Fischer et al. 2023)

Zoom-in on embedded stars

Küffmeier et al.

2019

Küffmeier et al. 2018

Küffmeier, Reißl et al. 2020

bridge structure similar to IRAS 16293--2422 (e.g. Sadavoy+ 2018, van der Wiel+ 2019, Maureira+ 2020)

~1500 AU

realistic initial conditions!

WIP: study synthetic observations of infall-induced shadows

RGB image of misaligned system forming from infall with 60°

blue (1.66 micron), green (53 micron), red (870 micron); Credit: S. Reißl

Effect of infall angle on disk

Formation of misaligned configuration

Observable as shadows in outer disk

Ginski et al. 2021