Catherine Espaillat, Mayra Osorio, Guillem Anglada, José M ......MULTI-WAVELENGTH CHARACTERIZATION OF RING SUBSTRUCTURES IN HD 169142 ENRIQUE MACIAS (Boston University) Catherine

MULTI-WAVELENGTH CHARACTERIZATION OF RING SUBSTRUCTURES IN HD 169142

ENRIQUE MACIAS (Boston University) Catherine Espaillat, Mayra Osorio, Guillem Anglada, José M. Torrelles, Carlos Carrasco-González, Mario Flock, Hendrik Linz, Gesa Bertrang, Thomas Henning, José F. Gómez, Nuria Calvet, Bill Dent

DISK SUBSTRUCTURES IN THE PLANET FORMATION PARADIGM

▸ Disk substructures are mostly ubiquitous (e.g., talks by J. Huang, G. Herczeg, L. Pérez).

‣ Could be a key piece of the dust evolution process:

Maximum particle size of ~1 m

Solution: non-smooth gas distributions

i.e., pressure bumps to trap the dust.

Dust radial drift + fragmentation

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ARE SUBSTRUCTURES THE SMOKING OF DUST TRAPS? �3

Substructures

Dust trap‣ Planet-disk interaction (e.g., Zhu et al.

2014).

‣ MHD effects (e.g., Flock et al. 2015)

No pressure bump

‣ Grain growth across snowlines (e.g., Pinilla et al. 2017)

‣ Dust sintering (Okuzumi et al. 2016)

THE ORIGIN AND ROLE OF DISK SUBSTRUCTURES

Characterizing dust content of substructures is key to understand their origin and role.

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Multi-wavelength observations in the (sub-)mm

‣ Are disk substructures the smoking gun of dust traps?

‣ Are substructures enhancing the dust growth?

HD 169142

Macias et al. (2017)

SPHERE J band

Pohl et al. (2017)

Fedele et al.

ALM 1.3

Talk by S. Pérez; Pérez et al. (2019)

ALMA 1.3 mm

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MULTI-WAVELENGTH ALMA OBSERVATIONS

Macias et al. in press

‣Archival band 7 (0.89 mm) and 6 (1.3 mm) data.

‣New band 3 (3 mm) observations.

‣Angular Resolution ~0.1 arcsec (~12 au)

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0.89 mm

3 mm

B1 B2 B3 B4B1 B2 B3 B4 B1 B2 B3 B4

�70.89 mm

MULTI-WAVELENGTH ANALYSISSpectral behavior of dust opacity depends on the dust particle size distribution.

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� ⇠ 0� 1<latexit sha1_base64="auQDr69fkb6CVgCa7Au/HsmW3K8=">AAAB+XicbVBNS8NAEJ34WetX1KOXxSJ4sSRV0GPRi8cK9gOaUDbbTbt0dxN2N4US+k+8eFDEq//Em//GbZuDtj4YeLw3w8y8KOVMG8/7dtbWNza3tks75d29/YND9+i4pZNMEdokCU9UJ8KaciZp0zDDaSdVFIuI03Y0up/57TFVmiXyyUxSGgo8kCxmBBsr9Vw3iKjBKNBMIA9dIr/nVryqNwdaJX5BKlCg0XO/gn5CMkGlIRxr3fW91IQ5VoYRTqflINM0xWSEB7RrqcSC6jCfXz5F51bpozhRtqRBc/X3RI6F1hMR2U6BzVAvezPxP6+bmfg2zJlMM0MlWSyKM45MgmYxoD5TlBg+sQQTxeytiAyxwsTYsMo2BH/55VXSqlX9q2rt8bpSvyviKMEpnMEF+HADdXiABjSBwBie4RXenNx5cd6dj0XrmlPMnMAfOJ8/EKKR+g==</latexit>

ISM-size

mm/cm

Dust opacity:

⌧⌫ [r] = ⌧0[r]

✓⌫

⌫0

◆�[r]

<latexit sha1_base64="ehQSdqvgDg7DV4/ohzKAGdvhYkI=">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</latexit>

‣ Gray body: I⌫ [r] = B⌫(Td[r]) (1� e⌧⌫ [r]))<latexit sha1_base64="ttlrxwMU2tUYHZxyJXmoNuo4xU4=">AAACHHicbVBLSwMxGMz6rPW16tFLsAjtwbLbCnoRSr3orUJf0F2XbDZtQ7PZJckKZan/w4t/xYsHRbx4EPw3pg9EWwcCk5n5SL7xY0alsqwvY2l5ZXVtPbOR3dza3tk19/abMkoEJg0csUi0fSQJo5w0FFWMtGNBUOgz0vIHl2O/dUeEpBGvq2FM3BD1OO1SjJSWPLN87aUOT0Yd4cILWJ1e8nUv0ELhPm+fkNvUUSj5SY0KBc/MWUVrArhI7BnJgRlqnvnhBBFOQsIVZkjKjm3Fyk2RUBQzMso6iSQxwgPUIx1NOQqJdNPJciN4rJUAdiOhD1dwov6eSFEo5TD0dTJEqi/nvbH4n9dJVPfcTSmPE0U4nj7UTRhUERw3BQMqCFZsqAnCguq/QtxHAmGl+8zqEuz5lRdJs1S0y8XSzWmuUp3VkQGH4AjkgQ3OQAVcgRpoAAwewBN4Aa/Go/FsvBnv0+iSMZs5AH9gfH4Dm/ShFA==</latexit>

MULTI-WAVELENGTH ANALYSISSpectral behavior of dust opacity depends on the dust particle size distribution.

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� ⇠ 0� 1<latexit sha1_base64="auQDr69fkb6CVgCa7Au/HsmW3K8=">AAAB+XicbVBNS8NAEJ34WetX1KOXxSJ4sSRV0GPRi8cK9gOaUDbbTbt0dxN2N4US+k+8eFDEq//Em//GbZuDtj4YeLw3w8y8KOVMG8/7dtbWNza3tks75d29/YND9+i4pZNMEdokCU9UJ8KaciZp0zDDaSdVFIuI03Y0up/57TFVmiXyyUxSGgo8kCxmBBsr9Vw3iKjBKNBMIA9dIr/nVryqNwdaJX5BKlCg0XO/gn5CMkGlIRxr3fW91IQ5VoYRTqflINM0xWSEB7RrqcSC6jCfXz5F51bpozhRtqRBc/X3RI6F1hMR2U6BzVAvezPxP6+bmfg2zJlMM0MlWSyKM45MgmYxoD5TlBg+sQQTxeytiAyxwsTYsMo2BH/55VXSqlX9q2rt8bpSvyviKMEpnMEF+HADdXiABjSBwBie4RXenNx5cd6dj0XrmlPMnMAfOJ8/EKKR+g==</latexit>

ISM-size

mm/cm

Dust opacity:

⌧⌫ [r] = ⌧0[r]

✓⌫

⌫0

◆�[r]

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Td[r]<latexit sha1_base64="wZf5ke/X/OYv4JO/B+tgRo2RJyE=">AAAB7XicbVBNS8NAEJ3Ur1q/qh69LBbBU0mqoMeiF48V2lpIQ9lsNu3azW7Y3Qgl9D948aCIV/+PN/+N2zYHbX0w8Hhvhpl5YcqZNq777ZTW1jc2t8rblZ3dvf2D6uFRV8tMEdohkkvVC7GmnAnaMcxw2ksVxUnI6UM4vp35D09UaSZF20xSGiR4KFjMCDZW6rYHka+CQbXm1t050CrxClKDAq1B9asfSZIlVBjCsda+56YmyLEyjHA6rfQzTVNMxnhIfUsFTqgO8vm1U3RmlQjFUtkSBs3V3xM5TrSeJKHtTLAZ6WVvJv7n+ZmJr4OciTQzVJDFojjjyEg0ex1FTFFi+MQSTBSztyIywgoTYwOq2BC85ZdXSbdR9y7qjfvLWvOmiKMMJ3AK5+DBFTThDlrQAQKP8Ayv8OZI58V5dz4WrSWnmDmGP3A+fwBaY477</latexit>

⌧0[r]<latexit sha1_base64="O0ktWykytvA//An3kxhk0LgYbzI=">AAAB8HicbVBNS8NAEJ3Ur1q/qh69LBbBU0mqoMeiF48V7IekoWy2m3bpbhJ2J0Ip/RVePCji1Z/jzX/jts1BWx8MPN6bYWZemEph0HW/ncLa+sbmVnG7tLO7t39QPjxqmSTTjDdZIhPdCanhUsS8iQIl76SaUxVK3g5HtzO//cS1EUn8gOOUB4oOYhEJRtFKj12kWc/1ddArV9yqOwdZJV5OKpCj0St/dfsJyxSPkUlqjO+5KQ YTqlEwyaelbmZ4StmIDrhvaUwVN8FkfvCUnFmlT6JE24qRzNXfExOqjBmr0HYqikOz7M3E/zw/w+g6mIg4zZDHbLEoyiTBhMy+J32hOUM5toQyLeythA2ppgxtRiUbgrf88ipp1areRbV2f1mp3+RxFOEETuEcPLiCOtxBA5rAQMEzvMKbo50X5935WLQWnHzmGP7A+fwBgySQNw==</latexit>

�[r]<latexit sha1_base64="8N/NswOtwrY0g6+OEntQtqSWzMU=">AAAB73icbVBNS8NAEJ3Ur1q/qh69LBbBU0mqoMeiF48V7Ae0oWy2k3bpZhN3N0IJ/RNePCji1b/jzX/jts1BWx8MPN6bYWZekAiujet+O4W19Y3NreJ2aWd3b/+gfHjU0nGqGDZZLGLVCahGwSU2DTcCO4lCGgUC28H4dua3n1BpHssHM0nQj+hQ8pAzaqzU6QVoaFf5/XLFrbpzkFXi5aQCORr98ldvELM0QmmYoFp3PTcxfkaV4UzgtNRLNSaUjekQu5ZKGqH2s/m9U3JmlQEJY2VLGjJXf09kNNJ6EgW2M6JmpJe9mfif101NeO1nXCapQckWi8JUEBOT2fNkwBUyIyaWUKa4vZWwEVWUGRtRyYbgLb+8Slq1qndRrd1fVuo3eRxFOIFTOAcPrqAOd9CAJjAQ8Ayv8OY8Oi/Ou/OxaC04+cwx/IHz+QP+xI/w</latexit>

Power law

Power law + 3 rings

MCMC

+ inclination, PA, position offsets

‣ Gray body:

RINGS AS ACCUMULATIONS OF PEBBLES �10

‣ The three rings are reproduced with increases in optical depth and decreases in beta accumulations of large dust grains.


‣ The three rings are reproduced with increases in optical depth and decreases in beta accumulations of large dust grains.

‣ We can discard snowlines as a main driver of substructures.

‣ Rings are likely associated with pressure bumps.

‣ Disk probably harbors multiple giant planets (Pohl et al. 2017; Bertrang et al. 2018).

RINGS AS ACCUMULATIONS OF PEBBLES �11


DUST PARTICLE SIZE DISTRIBUTION‣ Dust opacities as in DSHARP (Birnstiel et al. 2018) and n(a) / a�p

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⌧0<latexit sha1_base64="fCxjq/toupiVcNz5ScxXjJcTmQc=">AAAB7XicbVBNS8NAEJ3Ur1q/qh69LBbBU0mqoMeiF48V7Ae0oWy2m3btZhN2J0IJ/Q9ePCji1f/jzX/jts1BWx8MPN6bYWZekEhh0HW/ncLa+sbmVnG7tLO7t39QPjxqmTjVjDdZLGPdCajhUijeRIGSdxLNaRRI3g7GtzO//cS1EbF6wEnC/YgOlQgFo2ilVg9p2nf75Ypbdecgq8TLSQVyNPrlr94gZmnEFTJJjel6boJ+RjUKJvm01EsNTygb0yHvWqpoxI2fza+dkjOrDEgYa1sKyVz9PZHRyJhJFNjOiOLILHsz8T+vm2J47WdCJSlyxRaLwlQSjMnsdTIQmjOUE0so08LeStiIasrQBlSyIXjLL6+SVq3qXVRr95eV+k0eRxFO4BTOwYMrqMMdNKAJDB7hGV7hzYmdF+fd+Vi0Fpx85hj+wPn8AUjHju8=</latexit>

�12

Dust surface density:

Size distribution slope:

Max grain size:

DUST PARTICLE SIZE DISTRIBUTION‣ Dust opacities as in DSHARP (Birnstiel et al. 2018) and n(a) / a�p

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p<latexit sha1_base64="YCRLqY3FYFMPr169IIibebwVZHg=">AAAB6HicbVBNS8NAEJ3Ur1q/qh69LBbBU0mqoMeiF48t2FpoQ9lsJ+3azSbsboQS+gu8eFDEqz/Jm//GbZuDtj4YeLw3w8y8IBFcG9f9dgpr6xubW8Xt0s7u3v5B+fCoreNUMWyxWMSqE1CNgktsGW4EdhKFNAoEPgTj25n/8IRK81jem0mCfkSHkoecUWOlZtIvV9yqOwdZJV5OKpCj0S9/9QYxSyOUhgmqdddzE+NnVBnOBE5LvVRjQtmYDrFrqaQRaj+bHzolZ1YZkDBWtqQhc/X3REYjrSdRYDsjakZ62ZuJ/3nd1ITXfsZlkhqUbLEoTAUxMZl9TQZcITNiYgllittbCRtRRZmx2ZRsCN7yy6ukXat6F9Va87JSv8njKMIJnMI5eHAFdbiDBrSAAcIzvMKb8+i8OO/Ox6K14OQzx/AHzucP22eM+A==</latexit> 0

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⌃d<latexit sha1_base64="JFfMmCXxoEp/z9qahys76pDmlH4=">AAAB73icbVBNSwMxEJ2tX7V+VT16CRbBU9mtBT0WvXisaD+gXUo2m21Dk+yaZIWy9E948aCIV/+ON/+NabsHbX0w8Hhvhpl5QcKZNq777RTW1jc2t4rbpZ3dvf2D8uFRW8epIrRFYh6rboA15UzSlmGG026iKBYBp51gfDPzO09UaRbLBzNJqC/wULKIEWys1O3fs6HAg3BQrrhVdw60SrycVCBHc1D+6ocxSQWVhnCsdc9zE+NnWBlGOJ2W+qmmCSZjPKQ9SyUWVPvZ/N4pOrNKiKJY2ZIGzdXfExkWWk9EYDsFNiO97M3E/7xeaqIrP2MySQ2VZLEoSjkyMZo9j0KmKDF8YgkmitlbERlhhYmxEZVsCN7yy6ukXat6F9XaXb3SuM7jKMIJnMI5eHAJDbiFJrSAAIdneIU359F5cd6dj0VrwclnjuEPnM8f4x+P3g==</latexit>


�13

Dust surface density:

Size distribution slope:

Max grain size: ‣ Dust mass = ‣ Maximum grain size: 2 mm - 20 cm ‣ p = 3.5 in gaps (ISM-like)

160+250�90 M�

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INNER RING HARBORS A STRONG BUILD-UP OF LARGE PARTICLES �14

‣ Max grain size ~1 cm ‣ Slope p~1.5 ‣ dust-to-gas mass ratio ~ 1

(with from Fedele et al. 2017).⌃g<latexit sha1_base64="sFzEt2z46OqIGZNian+Itr4lZOQ=">AAAB73icbVBNSwMxEJ2tX7V+VT16CRbBU9mtBT0WvXisaD+gXUo2zW5Dk+yaZIWy9E948aCIV/+ON/+NabsHbX0w8Hhvhpl5QcKZNq777RTW1jc2t4rbpZ3dvf2D8uFRW8epIrRFYh6rboA15UzSlmGG026iKBYBp51gfDPzO09UaRbLBzNJqC9wJFnICDZW6vbvWSTwIBqUK27VnQOtEi8nFcjRHJS/+sOYpIJKQzjWuue5ifEzrAwjnE5L/VTTBJMxjmjPUokF1X42v3eKzqwyRGGsbEmD5urviQwLrScisJ0Cm5Fe9mbif14vNeGVnzGZpIZKslgUphyZGM2eR0OmKDF8YgkmitlbERlhhYmxEZVsCN7yy6ukXat6F9XaXb3SuM7jKMIJnMI5eHAJDbiFJrSAAIdneIU359F5cd6dj0VrwclnjuEPnM8f56uP4Q==</latexit>

‣ Streaming instability? ‣ Scattering?

‣ ~ 0.7 ‣ ~ 0.25




SUMMARY & CONCLUSIONS▸ ALMA ~0.1” (~12 au) data at 0.89 mm, 1.3 mm, and 3 mm of HD 169142.

▸ Discard: snowlines as the origin of main substructures in HD 169142.

▸ Confirm: substructures are associated with pressure bumps trapping large particles: potential sites for further planetesimal formation.

▸ Inner ring might contain appropriate conditions for streaming instability.

▸ Future prospects: • More targets. • More resolution: Cycle 6 ~0.05” @ 3 mm (PI: Macias). • (More) scattering. • More wavelengths: VLA.

�15

THANKS!

Documents

Catherine Espaillat, Mayra Osorio, Guillem Anglada, José M ......MULTI-WAVELENGTH CHARACTERIZATION OF RING SUBSTRUCTURES IN HD 169142 ENRIQUE MACIAS (Boston University) Catherine