each combination between the two shapes, the bilobed shape and the shape 67P, and the two TPMs, model A and model α.

This ability is a characteristic of the domain decomposition.

For lowestenergy states and sublimation following an instantaneous TPM, each region is related to torque formation pointing into one of the eight spatial quadrants with respect to the solar basis.

Each region collects one specific combination of (signs for) the vectorial torque efficiency.

Thus, the weights of the effective active fraction control all torque directions.

Eight is the minimum number for weights (and regions), and it is obtained by our approach.

On the surface of comet 67P/C-G for a wide range of locations, the weights for effective active fraction are not well constrained by rotation data.

This indetermination stems from the specifics of both, the geometry of the nucleus and the activity model.

We have shown this comparing results for two shapes and two activity models.

A better localization of the activity must consider complementary data.

Attree et al. (2023) shows the op-
nificant limitations.

The only region in which all the setups agree is A1,1,1 ⊂ASH with weights in the range 0.06 ≤fEAF,1,1,1 ≤0.08.

This is related to the fact that the data in Sect. 2.4 describe the dynamics for negative SSL (during the perihelion passage of comet 67P/C-G in 2015) predominantly and thus for activity on ASH.

In Fig. 6 for the shape 67P, A1,1,1 is located in the regions (0◦, 60◦)×(−90◦, −45◦) and (150◦, 210◦)×(−90◦, −30◦) for λ and ϕ.

This fits well with the location of increased activity in Fig. 10 of Kramer et al. (2019).

The same authors report a decrease in the effective active fraction in the regions (−45◦, 15◦)×(−30◦, 0◦) and (150◦, 210◦) × (−15◦, 15◦) for λ and ϕ.

This statement correlates to reduced weights in Fig. 13 for the regions A−1,−1,−1 and A1,−1,1 in Fig. 6.

Restricted to model A, some agreement can be obtained between the two shapes on the regions A−1,−1,−1, A1,1,−1, and A−1,−1,1.

On the remaining regions the weights contain much
higher uncertainties based on the consideration of all different setups.

One major difference between the evolutions of uniform (Fig. 12) and weighted (Fig. 14) activity is the rotated trajectory for the two ω directions.

For uniform activity, Fig. 11 shows this trajectory (with respect to the solar basis) close to the line λs = −90◦.

For weighted activity, Fig. 15 shows the same trajectory close to the line λs = 0◦.

Especially for negative SSLs (related to the early part of the evolution in Fig. 15), weighted activity causes this rotation for the ω trajectory (and for the slope along the trajectory) by approximately 90◦.

Negative SSLs represent predominant illumination conditions during the perihelion passage of comet 67P/C-G in 2015.

Due to rotation states close to lowest energy, this directional change applies to L as well.

For weighted activity, the torque, T, points mainly in the λs = 0◦ direction that expresses T · b1 > 0.

Thus this directional evolu-
tion in Fig. 15 confirms the increased weights for region A1,1,1 in

[Figure: Fig. 13.]

Article number, page 12 production such as in Läuter et al.