Filling the gap Asteroids with slow rotation in thermal infrared A. - - PowerPoint PPT Presentation

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Filling the gap Asteroids with slow rotation in thermal infrared A. - - PowerPoint PPT Presentation

Dec 12, 2023 132 likes •322 views

Selection effects Shape models TPM Results Summary Filling the gap Asteroids with slow rotation in thermal infrared A. Marciniak 1 , V. Al-Lagoa, T. Mller, P . Bartczak R. Behrend, M. Butkiewicz-B ak, G. Dudzi nski, R. Duffard, K.

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SLIDE 1

Selection effects Shape models TPM Results Summary

Filling the gap Asteroids with slow rotation in thermal infrared

  • A. Marciniak1, V. Alí-Lagoa, T. Müller, P

. Bartczak

  • R. Behrend, M. Butkiewicz-B ˛

ak, G. Dudzi´ nski, R. Duffard, K. Dziadura,

  • S. Fauvaud, S. Geier, J. Grice, R. Hirsch, J. Horbowicz, K. Kami´

nski, P . Kankiewicz, D.-H. Kim, M.-J. Kim, I. Konstanciak, V. Kudak, L. Molnár,

  • F. Monteiro, W. Ogłoza, D. Oszkiewicz, A. Pál, N. Parley, F. Pilcher, E. Podlewska -

Gaca, T. Polakis, J. J. Sanabria, T. Santana-Ros, B. Skiff, K. Sobkowiak,

  • R. Szakáts, S. Urakawa, M. ˙

Zejmo, K. ˙ Zukowski

  • 1. Astronomical Observatory Institute, Faculty of Physics, A. Mickiewicz University,

Pozna´ n, Poland.

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SLIDE 2

Selection effects Shape models TPM Results Summary

Selection effects in MBA models

All 1230 asteroids with H≥11 mag Division values: P = 12 h, amax = 0.25 mag.

Marciniak et al. 2018

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Selection effects Shape models TPM Results Summary

Selection effects in fainter MBA models

All 2274 asteroids with 11 < H≤ 13 mag Division values: P = 12 h, amax = 0.25 mag.

Marciniak et al. 2018

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SLIDE 4

Selection effects Shape models TPM Results Summary

Selected lightcurves

0,1 0,2 0,3 0,4 0,5 0,6 0,7 0,8 0,9 1 Phase

  • 3,3
  • 3,2
  • 3,1

Relative C magnitude

29 Sep, Bor. 18 Oct, Organ M. 19 Oct, Bor. 19 Oct, Organ M. 25 Oct, Bor. 21 Nov, Organ M. 18 Dec, Organ M. 23 Dec, Bor.

335 Roberta

P=12.027 h Zero time at: 2013 Sep 28.9158 UTC, LT corr. 2013 0,1 0,2 0,3 0,4 0,5 0,6 0,7 0,8 0,9 1 Phase 8,35 8,4 8,45 8,5 8,55 8,6 8,65 Relative R magnitude

Feb 1.1 Kepler Feb 2.1 Kepler Feb 3.3 Kepler Feb 4.0 Kepler Feb 5.0 Kepler Feb 5.9 Kepler May 19.1 Kepler May19.8 Kepler May 20.8 Kepler May 21.8 Kepler May 22.5 Kepler

100 Hekate

P=27.068 h Zero time at: 2018 Jan 31.7150 UTC, LT corr. 2018 0,1 0,2 0,3 0,4 0,5 0,6 0,7 0,8 0,9 1 Phase

  • 4,5
  • 4,4
  • 4,3
  • 4,2

Relative C and R magnitude

Jan 22.3 CTIO Jan 27.1 Bor. Jan 29.1 Bor. Feb 16.1 Bor. Feb 22.4 Tempe Feb 23.4 Tempe Feb 24.4 Tempe Feb 25.4 Tempe Feb 27.4 Tempe Mar 1.4 Tempe

109 Felicitas

P = 13.188 h Zero time at 2017 Jan 28.9650 UTC, LT corr. 2017 0,1 0,2 0,3 0,4 0,5 0,6 0,7 0,8 0,9 1 Phase

  • 3,5
  • 3,4
  • 3,3
  • 3,2
  • 3,1

Relative R and C magnitude

Oct 18.1 Bor. Oct 19.0 Bor. Nov 1.1 Bor. Nov 4.1 OAdM Nov 6.1 Bor. Nov 7.1 Bor. Nov 10.4 Organ M. Nov 17.4 Organ M. Nov 18.0 Bor. Nov 29.3 Organ M. Dec 5.9 Bor. Dec 11.2 OAdM Dec 14.3 Organ M.

538 Friederike

P=46.74 h Zero time at: 2018 Oct 17.9492 UTC, LT corr. 2018

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Selection effects Shape models TPM Results Summary

Fitting the shape models to stellar occultation chords

Diameters of equivalent volume sphere: CONVEX (2011): 72 ± 4 km; CONVEX (2013): 74 ± 5 km SAGE (2011): 70 ± 4 km; SAGE (2013): 72 ± 3 km Marciniak et al. 2018

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Selection effects Shape models TPM Results Summary

Thermophysical modelling

Insolation and surface temperature distribution: (159) Aemilia

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Selection effects Shape models TPM Results Summary

O-C plots for (159) Aemilia model applied in TPM

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Selection effects Shape models TPM Results Summary

Rotation Radiometric solution for combined data. Target period Taxonomic Diameter Albedo Thermal inertia [h] type [km] [Jm−2s−0.5K−1] 159 Aemilia 24.4787 Ch 137 0.054 50 ±0.0001 ±8 ±0.015 ±50 227 Philosophia 26.4614 C 101 0.041 125 ±0.0001 ±5 ±0.005 ±90 329 Svea 22.7670 C 78 0.055 75 ±0.0001 ±4 ±0.015 ±50 478 Tergeste 16.10312 L 87 0.15 75 ±0.00003 ±6 ±0.02 ±45 487 Venetia 13.34133 S 70 0.21 100 ±0.00002 ±4 ±0.02 ±75

Marciniak et al. 2018

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Selection effects Shape models TPM Results Summary

Thermal inertia of Main Belt Asteroids

Harris & Drube 2016

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Selection effects Shape models TPM Results Summary

Thermal inertia of slow rotators

after: Harris & Drube 2016

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Selection effects Shape models TPM Results Summary

(195) Eurykleia model in thermophysical modelling

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SLIDE 12

Selection effects Shape models TPM Results Summary

Thermal lightcurve fit to WISE W4 data (target: 673 Edda)

1 1.1 1.2 1.3 1.4 1.5 1.6 1.7 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1 Flux (Jy) Rotational phase W4 data Best fit AM 1

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Selection effects Shape models TPM Results Summary

O-C plots for (673) Edda model applied in TPM

0.5 1 1.5 2 10 100 Obs/Mod Wavelength (micron) AM 1 20 40 60 80 100 120 140 160 180 Aspect angle (deg.) 0.5 1 1.5 2

  • 40
  • 30
  • 20
  • 10

10 20 30 40 Obs/Mod Phase angle (degree) AM 1 10 20 30 40 50 60 Wavelength (micron) 0.5 1 1.5 2 2.805 2.81 2.815 2.82 2.825 2.83 2.835 2.84 2.845 Obs/Mod Heliocentric distance (au) AM 1 10 20 30 40 50 60 Wavelength (micron) 0.5 1 1.5 2 0.2 0.4 0.6 0.8 1 Obs/Mod Rotational phase AM 1 20 40 60 80 100 120 140 160 180 Aspect angle (deg.)

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Selection effects Shape models TPM Results Summary

Summary of TPM results for (673) Edda.

Shape model IR data subset ¯ χ2

m

D ± 3σ (km) Γ ± 3σ (SIu) Roughness (rms) AM 1 All data 0.47 38+6

−2

3+67

−3

Med.-high (0.50) AM 1 sphere All data 1.83 38 5 Med.-high (0.39) AM 2 All data 0.59 382+

−2

3+37

−3

  • Extr. high (1.0)

AM 2 sphere All data 1.76 38 10. Medium (0.44)

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Selection effects Shape models TPM Results Summary

Rotation Radiometric solution for combined data. Target period Taxonomic Diameter Albedo Thermal inertia [h] type [km] [SI units] 100 Hekate 27.07027 S 87+5

−4

0.22+0.03

−0.03

4+66

−2

±0.00006 109 Felicitas 13.190550 Ch 85+7

−5

0.065+0.008

−0.01

40+100

−36

±0.000004 195 Eurykleia 16.52178 Ch 87+11

−9

0.06±0.02 15+55

−15

±0.00002 301 Bavaria 12.24090 C 55+2

−2

0.047+0.004

−0.003

45+60

−30

±0.00001 335 Roberta 12.02713 B 98+10

−11

0.046+0.014

−0.008

unconstrained ±0.00003 380 Fiducia 13.71723 C 72+9

−5

0.057+0.009

−0.012

10+140

−10

±0.00002 468 Lina 16.47838 CPF 69+11

−4

0.052+0.006

−0.014

20+280

−20

±0.00003 538 Friederike 46.739 C 77+4

−2

0.06±0.01 10+25

−10

±0.001 653 Berenike 12.48357 K 46+4

−2

0.18+0.02

−0.03

40+120

−40

±0.00003 673 Edda 22.33411 S 38+6

−2

0.13+0.03

−0.05

3+67

−3

±0.00004 834 Burnhamia 13.87594 GS 67+8

−6

0.074+0.014

−0.016

20+30

−20

±0.00002

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Selection effects Shape models TPM Results Summary

Thermal inertia of slow rotators

after: Harris & Drube 2016

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Selection effects Shape models TPM Results Summary

Thermal inertia normalised to 1 AU vs. size

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Selection effects Shape models TPM Results Summary

Summary

Selection effects: spin and shape models mainly available for short-period, elongated asteroids with extreme obliquities Biased spatial spin axis and size-frequency distributions, lack of detailed models for slow rotators Our targeted survey of 100 long-period, low-amplitude MB asteroids. Gathered over 10 000 hours of lightcurve data in 20 stations worldwide (+ Kepler). Modelled 16 targets from this sample, scaled by TPM using IR data from IRAS, AKARI and WISE Found high, medium and very low thermal inertias Differences due to sub-surface temperatures and different material properties? Indication of fresh and old surfaces connected with formation age and/or size?

This work was supported by grant no. 2014/13/D/ST9/01818 from National Science Centre, Poland. The research leading to these results has received funding from the European Union’s Horizon 2020 Research and Innovation Programme, under Grant Agreement no 687378.