© The Authors 2024

1. Introduction

Our Solar System (SolS) is located in a relatively calm region of the Galaxy, namely, between two spiral arms (Perseus and Scutum-Centaurus) at a distance of ≈8 kpc from the centre of the Galaxy. During the analysis of globular cluster (GC) orbits in our previous paper Ishchenko et al. (2023a, hereafter, Paper I), we found that more than 50 GCs can potentially cross the orbital trajectory of the Sun. In our following paper, we concluded that even a “collision” between two GCs is not a unique phenomenon (Ishchenko et al. 2023b). Globular clusters are objects that can even actively interact with the Galactic centre (Ishchenko et al. 2023c), open clusters (de la Fuente Marcos et al. 2014), and with each other (Khoperskov et al. 2018; Ishchenko et al. 2023b). Thus, we assume that close passages of individual stars could have a gravitational influence not only on SolS dynamics (de la Fuente Marcos & de la Fuente Marcos 2022; Portegies Zwart 2021; Portegies Zwart et al. 2021; Bailer-Jones 2022) and star clusters (Pfalzner & Vincke 2020; Pfalzner et al. 2021; Pfalzner & Govind 2021) but potentially also on a whole GC as well.

In this paper, our aim is to investigate the possible gravitational influence of close passages of GCs on the SolS. Our main tasks can be formulated as follows: performing statistical analysis of the total interaction of GCs with the SolS, estimating the interaction and probability of close passages near the SolS for individual GCs, and estimating the gravitational influence onto the Oort cloud due to the potential close passages of GCs.

To add more realism to our dynamical orbital evolution (simulations), we added to the standard N-body code the time-dependent external potentials, which were selected from IllustrisTNG-100 cosmological simulation database (Nelson et al. 2018, 2019a,b). We selected five IllustrisTNG time variable potentials (TNG-TVP) that (at present redshift z = 0) have parameters (halo and disc masses, and their characteristic scales) similar to our present day Galaxy: 411321, 441327, 451323, 462077, and 474170. The procedure for sampling and fitting the selected potentials is described in detail in the papers Paper I and Mardini et al. (2020). The code routines are also publicly available at GitHub¹. As a typical example, we present the main parameters (halo and disc masses, and their characteristic scales) for 411321 TNG-TVP in Table 1. For a more detailed description of all five selected TNG-TVP, we refer to our previous Paper I.

In addition to our five selected TNG-TVPs, we added another fixed potential whose parameters (such as halo, disc, and bulge masses, and their characteristic scales) do not change over time. We refer to this potential using the code-name “FIX”. For this potential in our simulations, we used the three-component (bulge-disc-halo) axisymmetric Plummer–Kuzmin model (Miyamoto & Nagai 1975), as in Just et al. (2009) and Shukirgaliyev et al. (2021). We present the parameters (halo and disc masses, and their characteristic scales) for TNG external and static potentials in Table 1.

As an initial condition for our GC system, we used the randomised 6D phase-space orbital information provided from Baumgardt & Vasiliev (2021)². Using 1000 initial data sets for each potential, in total we obtained 6000 runs for the GC systems in the integration procedure. More details about the dynamical integration can be found in our previous papers, Ishchenko et al. (2023b,c).

To reproduce the orbit of the Sun in the past, we accepted an in-plane distance of the Sun from the Galactic centre at the plane as X_⊙ = 8.178 kpc (GRAVITY Collaboration 2019), Z_⊙ = 20.8 pc (Bennett & Bovy 2019). The velocity transformation is basically described in Johnson & Soderblom (1987), but for the equatorial position of the North Galactic Pole (NGP), we used the updated values from Karim & Mamajek (2017): RA${}_{\mathrm{NGP}}=192\stackrel{°}{.}7278$, Dec${}_{\mathrm{NGP}}=26\stackrel{°}{.}8630$, ${\theta }_{\mathrm{NGP}}=122\stackrel{°}{.}9280$. For the Local Standard of Rest (LSR) velocity, we set V_LSR = 234.737 km s⁻¹ (Reid & Brunthaler 2004), and for the peculiar velocity of the Sun with respect to the LSR, we used U_⊙ = 11.1 km s⁻¹, V_⊙ = 12.24 km s⁻¹, W_⊙ = 7.25 km s⁻¹ (Schönrich et al. 2010). Since the integration was performed backwards in time, the sign of the velocity components for Sun and GCs were changed to the opposite value.

Using these observations as initial conditions, we performed simulations of 147 GCs together with the Sun up to six billion years in look-back time. As we know, the age of the Sun is ∼5 Gyr since it is set on the main sequence (Bonanno et al. 2002; Connelly et al. 2012). We added an additional 1 Gyr in order to take into account some dynamical time for star formation itself.

The paper is organised as follows. In Sect. 2, we present the total interaction of the GCs with the SolS. In Sect. 3, we present the individual analysis of GC interaction. In Sects. 4 and 5, we present the gravity influence of GCs to the Oort cloud system and summarise our findings.

2. Total interaction of globular clusters with the Solar System

As a first step, we estimated all the close passage interactions of the GCs with the SolS. We used only one main criterion to characterise the close passages N_pass between the GCs and SolS, namely, the separation dR between the GC and SolS should be less than 200 pc. The close passages of typical GCs with masses on order of ∼10⁵ M_⊙ at such a distance can already have a strong gravitational influence on the outer part of the SolS (Portegies Zwart 2021; Portegies Zwart et al. 2021).

By analysing the results from all 6000 runs with the close passages that correspond to our criteria, we found only 56 GCs that have close passages near the SolS in at least one of the random realisations in one of the six selected potentials. Of these GCs, only 35 have close passages near the SolS in all the six potentials. Under our assumptions and taking into account the fact that in the used Gaia DR3 sample we have 147 GCs, in total we found that 38% of the 147 GCs could potentially have had close passages near the SolS during the whole six-billion-year evolution.

In Fig. 1 (left panel), we present the close passage interaction between GCs and SolS N_pass as a function of the relative distance dR for all the six potentials with all the individual randomisations for all 6000 runs in total. We present each potential in a different colour and averaged them over all the 1000 randomisations). The black dashed lines represent the linear fit for the corresponding potentials. Thus, we observed that the close passage interaction increases linearly with the relative distance between the GCs and SolS. The largest close passage interaction (N_pass) in the six billion years was obtained for 451323 TNG-TVP and in FIX potentials (blue and brown colours). We found the minimum number of close passages with the 462077 TNG-TVP potential (magenta colour).

Fig. 1. Average probability of the number of passages (left panel) between GCs and SolS as a function of the relative distance dR. The black dashed lines are the linear fit for the corresponding potentials. The right panel presents the average probability of the cumulative number of passages as a function of the minimum relative distance dR of the GCs at the moment of closest approach in all six potentials. Colours: 411321 – red, 441327 – green, 451323 – blue, 462077 – magenta, and 474170 – cyan. The brown colour is for the FIX potentials.

In Fig. 1 (right panel), we present the average probability of the cumulative number of passages as a function of the GCs’ minimum relative distance dR at the moment of closest approach to the SolS in all the six potentials (summed up for the 1000 randomisations). As can be seen, the resulting distribution as a function of dR is well fit by the simple power-law function:

$$\begin{array}{c}\hfill N_{\mathrm{pass}}(\mathrm{d}R)=\mathrm{b}·{(\mathrm{d}R)}^a,\end{array}$$(1)

where a = 1.99 ± 0.13 is the average best-fit slope parameter among our six variants of external potentials.

As can be seen, the of the cumulative close passage can be described by a simple quadratic relation: N_pass ∼ (dR)². By analysing Fig. 1 (right panel), for example, we can conclude that at a relative distance of 50 pc between a GC and the SolS, we get on average ∼15% of the close passage probability over all six billion years, and at dR = 100 pc, we get on average ∼35% of the close passage probability over all six billion years. In addition, Fig. 2 (right panel) presents the distribution of GC close passages N_pass near the SolS for all six potentials as a function of look-back time. The average probability, around 2–3%, is almost stable throughout the entire period of six billion years, except for the increase at the beginning (0–0.7 Gyr) and the decrease at the end (5.5–6 Gyr) of the integration.

Fig. 2. Relative velocities (left panel) and time when close passages happen (right panel) between the GCs and the SolS. Colours: 411321 – red, 441327 – green, 451323 – blue, 462077 – magenta, and 474170 – cyan. The brown colour is for the FIX potentials.

The main differences between the close encounter passages in Fig. 1 and the different external potentials can be explained based on the slightly different behaviour of our TNG-TVP potentials’ mass and size time evolution. For example, the encounter results for the potential 462077 are significantly lower compared to the other potentials. This can be explained as being due to the specific behaviour of the disc component scale lengths (a_d and b_d) in our last six billion years of look-back time (Paper I, see Fig. 2 therein). Interested readers can find a more detailed visualisation of all 159 GC orbits for different TNG-TVP potentials on the website of the project³.

In Fig. 2 (left panel), we present the velocity distribution for GCs that have close passages near the SolS. As can be seen, we found two groups with the first maximum around ∼200 km s⁻¹ and the second near the ∼300 km s⁻¹ (marked with black lines), where we have ∼7% of the probability of close passages. The main contribution in the first peak comes mainly from three clusters, BH 140, Djorg 1, and UKS 1, which have a close passage probability of more than ∼20%, on average, for the potentials. In the second peak, we have mainly the influence from the GCs that are in italics in the first block in Table A.1.

3. Individual analysis of the interaction of globular clusters with the Solar System

As a second step, we estimated the individual GC interaction with the SolS. In Table A.1, we present GCs that have close passages near the SolS divided across three blocks. In the first block, we present the selected 35 GCs that have close passages in all six potentials. In the second block are 8 GCs that have close passages in five potentials, and in the third are 6 GCs that have close passages only in four potentials. Also, in Table A.1, we present the kinematic parameters and properties such as the average minimum distance between the GC and the SolS (⟨dR_m⟩) in all potentials and their relative mean velocities at the moment of collision (⟨dV⟩). In Table A.1, we also present the current masses of the GCs and the half-mass radii as well as the type of orbit (TO), association of the Galaxy region (GR), and possible progenitor. The GCs IC 1276, NGC 5279, NGC 5466, NGC 6101, NGC 6333, NGC 4590, NGC 5034, and Pal 14 (eight GCs in total) are not presented in Table A.1 due to their extremely low collision probability (less than 0.1%) with the SolS and the full absence of such collisions in three or more potentials. In next paragraph, we present several conclusions about the selected GCs that have close passages near the SolS.

The GCs BH 140, UKS 1, and Djorg 1 have a mean minimum relative distance value of dR_m: 9 ± 5, 19 ± 6 and 17 ± 9 pc between the GC and the SolS over all six potentials. The average probability of these GCs’ interactions is ∼10% on average in each of our six potentials.

Of all the GCs, only a few, including NGC 2808, BH 140, Djorg 1, UKS 1, E 3, NGC 6656, and NGC 4833, have a statistically significant (10–20%) probability of interaction with the SolS in at least one of the six potentials across all six billion years. The other GCs presented in Table A.1 have a statistical probability from 5% to 9% over the six billion years. There were no close passages observed from the current day to 309 Myr in look-back time.

According to the possible progenitor classification of the GCs made by Massari et al. (2019) and Malhan et al. (2022), 22 GCs can be from Gaia-Enceladus (G-E), seven can be from Pontus (ex situ), and only in a third place we have five GCs that are within the Galaxy.

Most of our selected GCs have tube (TB) orbits, 23, or long radial (LR) orbits, 17, and the other nine GCs have irregular (IR) type orbits. These orbital classifications were performed in Paper I, according to Sect. 3.4 and Fig. 10 herein.

Also, in Fig. B.1, we present the Sun’s orbital evolution with the collision “points” with other GCs in the 411321 TNG external potential, which is presented in Table A.1. The colours of the circles are more intense if the area has a higher statistical value for collisions. As can be seen in the top panel of the figure, the intense magenta colour represents a statistical probability of more than 10% for NGC 7078. In the inner part of the Sun’s orbit, according to the R, we observed that close passages are more frequent than in the outer part of the orbit.

4. Influence of globular cluster gravity on the Oort cloud system

For the Oort cloud, the initial equilibrium particle distribution is the well-established (see Fig. 9 in Portegies Zwart et al. 2021) Dehnen profile (Dehnen 1993) with power slope γ = 2:

$$\begin{array}{c}\hfill {\rho }_{\mathrm{Oort}}(r)=\frac{(3-\gamma )·M_{\mathrm{Oort}}}{4\pi }\frac{a_{\mathrm{Oort}}}{r^{\gamma }{(r+a_{\mathrm{Oort}})}^{4-\gamma }},\end{array}$$(2)

where M_Oort is the total mass of the model Oort cloud (in our case 0.01 M_⊙), a_Oort is the Oort cloud scaling radius (which we set as 10⁵ au), and γ describes the inner power-law profile of the Dehnen model family (0 ≤ γ < 3).

For the actual data generation, we used the AGAMA library (Vasiliev 2019). The total mass of the Oort cloud we set initially equal to 1% M_⊙ (Portegies Zwart 2021). The inner and outer cut-off radii were set at 100 au (∼4.8 × 10⁻⁴ pc) and 1 pc (∼2 × 10⁵ au). For the outer radius truncation, we simply used the Sun Hill radius definition in the Galactic potential (which is around ∼1 pc, as in the Portegies Zwart 2021). The particle distribution generated around the Sun only takes into account the Sun’s gravitational field. As a basic model for our runs, we used N = 10 k Oort cloud particles.

In the next step, we had cloud particles around the Sun and adopted the Oort cloud system in the five external TNG-TVP Milky Way-like and FIX potentials. For the whole system, we set the Sun’s positions and velocities (see Sect. 1). Based on our Table A.1, we selected the set of GCs with close passage distances from the Sun (less than 20 pc) in all 1000 sets of randomisation and for all potentials (five TNG-TVP and FIX). We modified our basic code to calculate the self-gravity only between the Sun and the GC as particles. We neglected the self-gravity of the Oort cloud particles in our investigation, following Portegies Zwart et al. (2021). As an independent check of Oort cloud dynamical evolution, we ran the cloud plus Sun system without the GC perturbers for the 411321 TNG-TVP and FIX potentials. On these runs, the Oort cloud loses only ∼5% of particles (black lines in Fig. 3).

Fig. 3. Oort particle distributions due to gravitational influence of GCs. The different zones are as follows: Less than 2 pc – inner zone (top panel), from 2 pc to 1000 pc – middle zone (middle panel), and above 1000 pc – outer zone (bottom panel). The solid lines show the particle distribution, and dotted lines show moments of the GC deep passages. The colours represent potentials. The larger green dots represent the results with the N = 50 k Oort cloud number (re-scaled).

In Table 2, we present the list of selected GCs that came closer than 10 pc to the Sun. In Cols. 3 and 4 of the table, we present the minimal distance and time for when the GCs have a deep passage. To quantify the gravitational effect of GCs on the Oort cloud system, we defined ε_TID, IN, which we set as a ratio of the GC potential to the Sun potential acting on a cloud system inner radius (Col. 7 in the table):

$$\begin{array}{c}\hfill {\epsilon }_{\mathrm{TID},\mathrm{IN}}=\frac{{\mathrm{\Phi }}_{\mathrm{GC}}}{{\mathrm{\Phi }}_{\odot ,\mathrm{IN}}}=\frac{M_{\mathrm{GC}}[M_{\odot }]/r_{\mathrm{hm}}[\mathrm{pc}]}{1[M_{\odot }]/4.8\times {10}^{-4}[\mathrm{pc}]},\end{array}$$(3)

where M_GC is the GC mass and r_hm is the GC half-mass radius (respectively Cols. 5 and 6 in Table 2).

In this way, we basically defined the gravitational energetic influence of the GCs acting on the whole Oort cloud system. To estimate the potential from the GC due to the deep passage of the SolS into the GC, we defined the GC potential based on the cluster r_hm instead of using a point mass approximation.

We present a general overview of the interaction effect of the GCs in Fig. 3, which is related to Table 2. In this plot, for the analysis of the GC gravity influence on the Oort cloud particles, we established three zones based on the particle distances from the Sun: the inner part (R is up to 2 pc), between (R is from 2 to 1000 pc) and the outer part (R is above 1000 pc).

As can be seen from Table 2, NGC 7078 has a high gravitational influence on the Oort system. Notably, the close passages of NGC 7078 are twice as deep as those of 411321 and 462077 TNG-TVPs. But in the first case, this GC comes as close as 1 pc to the Sun and as close as 9 pc in the second. As we observed from Fig. 3, at the moment NGC 7078 had a close passage in 411321 (marked by a green dotted line at 0.33 Gyr), more than ∼30% of particles were immediately ejected from the first zone and moved to the second zone (green line). But in the case of 462077, at the relative distance of 9 pc, NGC 7078 did not have any influence on the Oort system (cyan line, T = 5.62 Gyr).

Another example of the gravitational energetic influence of GCs on the Oort system is NGC 6356 in the 474170 external potential. At the 1.2 pc distance, we had ε_TID, IN = 42 (magenta line, T = 0.34 Gyr), which caused ∼20% of the particles to move from the first zone to the second. But in the third zone (R above 1000 pc), this influence is almost negligible.

In the 451323 external potential, we have three GCs with deep close passages, and only two of them have a soft influence on the Oort system, namely, NGC 3201 and NGC 2808 (violet lines, T = 3.06 and 3.77 Gyr). Their influence is perceptible only in the first and second zones.

The GCs UKS 1, BH 140, and NGC 6426, and others that have masses less than ×10⁴ and have dR less than 4 pc do not have any gravitational influence on the Oort system (see Fig. 3, blue and red dotted lines). The NGC 6205 with ε_TID, IN = 50 in the 441327 potentially looks like an exception, though it does not have any effect on the Oort system either (T = 1.93 Gyr, red dotted line).

We performed additional calculations to evaluate the possible influence of the initial particle number in the Oort system on the obtained results. In this case, we prepared the initial distribution of the Oort cloud particles with the same physical conditions as in a previous case, but we changed the number of particles, increasing it to 50 k. Using these data, we carried out additional simulations with N = 50 k for the FIX and 411321 potentials. The time evolution of the Oort particle numbers in different zones for N = 10 k and 50 k and for 411321 TNG-TVP we compare in Fig. 3, re-scaled (divided by five). The green line represents the N = 10 k and the green dots represent the N = 50 k. As can be seen, there are no significant differences between these two runs. We had an absolutely similar time when the NGC 7078 comes inside the Oort system, and as a result, we observed the ejection of more than 30% of particles from the first zone to the second zone. After four billion years in look-back time, we observed small differences in the number of particles in the second and third zones that clearly reflect the result of the small particle numbers (especially in the third zone). We present the detailed distribution of the Oort cloud particles’ gravitational potentials for six billion years in look-back time in Fig. C.1.

5. Conclusions

After analysing the total interaction of GCs with the SolS, we found that close passages are not frequent but are also not exceptional events in the SolS lifetime. One can note that besides a quite different nature in the time variable of TNG-100 and FIX external potentials, the resulting close passage interaction of GCs with the SolS for these external potentials are surprisingly similar. For example, at a relative distance of 50 pc between a GC and the SolS, we obtained on average ∼15% of the close passage probability over all six billion years, and at dR = 100 pc, we got on average ∼35% of the close passage probability over all six billion years.

Summarising our set of calculations in Table 2 and Fig. 3, we observed that a potentially strong gravitational influence from deep close passages as close as a 1–2 pc on the Oort system would yield objects with typical masses above a few times 10⁵ M_⊙. Estimating the potential influence of the GCs on the SolS Oort clouds, we should expect that the GCs in the past could have had much higher masses and half-mass radii that would obviously lead to the stronger effects on the SolS.

Acknowledgments

The authors thank the anonymous referee for a very constructive report and suggestions that helped significantly improve the quality of the manuscript. M.I. and P.B. acknowledge the support within the grant No. AP14869395 of the Science Committee of the Ministry of Science and Higher Education of Kazakhstan (“Triune model of Galactic center dynamical evolution on cosmological time scale”). M.I., P.B., and M.S. thank the support from the special program of the Polish Academy of Sciences and the US National Academy of Sciences under the Long-term program to support Ukrainian research teams grant No. PAN.BFB.S.BWZ.329.022.2023. The work of M.I. was supported by the Grant of the National Academy of Sciences of Ukraine for young scientists. M.S. acknowledges the support under the Fellowship of the President of Ukraine for young scientists 2022–2024.

References

Appendix A: List of GCs with close passages near the Solar System

In Table A.1, we present the mean minimum relative distance (< dR_m> ) (minimum relative distance between GCs and SolS from each of our 6000 randomisations) and relative velocity (< dV> ) (also averaged by all randomisations). Column (5) of the table shows the first close passage end the relative distance at this moment, < T_l > ⇔ < dR>. In Columns (6) and (7), we present the GC’s current mass and half-mass radii. Column (8) shows the gravity influence on the Oort cloud system (rounded to the closest integer). To quantify the gravitational effect of a GC on the Oort cloud system, we re-defined the ε_TID, IN (see equation 3), which we set as a ratio of the GC potential to the Sun potential acting on a cloud system inner radius:

$$\begin{array}{c}\hfill {ϵ}_{\mathrm{TID},\mathrm{IN}}=\frac{{\mathrm{\Phi }}_{\mathrm{GC}}}{{\mathrm{\Phi }}_{\odot ,\mathrm{IN}}}=\frac{M_{\mathrm{GC}}[{\mathrm{M}}_{\odot }]/d{R}_{\mathrm{m}}[\mathrm{pc}]}{1[{\mathrm{M}}_{\odot }]/4.8·{10}^{-4}[\mathrm{pc}]},\end{array}$$(A.1)

where now we use the dR_m values from column (3) of the table and assume that the GC acts as a particle on the inner part of the Oort cloud system. Columns (9) and (10) show the type of GC orbits (TO) and different regions of the Galaxy (GR) at present, according to the classification from Bland-Hawthorn & Gerhard (2016). Column (11) shows the classification of the progenitors according to the Massari et al. (2019) and Malhan et al. (2022).

Appendix B: Orbital evolution of the Sun with the collision moments

As an example, we present the orbital evolution of the Sun with collision moments for several GCs: BH 140, UKS 1, Djorg 1, NGC 7078, NGC 2808. The colour points represents the counterparts of GC’s during the whole six-billion-years time interval.

Fig. B.1. Orbital Sun evolution with close passages during the whole integration time in 411321 TNG-TVP. Coloured circles: green for BH 140, red for UKS 1, blue for Djorg 1, magenta for NGC 7078, cyan for NGC 2808. The hollow circles outlined in grey are other GCs. The blue point is the start of integration. From top to bottom, the panels represent the interval of integration: 0 – 2 Gyr, 2 – 4 Gyr, and 4 – 6 Gyr in look-back time.

Appendix C: Oort particle distributions due to the GCs gravitational influence

In Fig. C.1 we present the gravitational potential acting on each Oort particle for each one-billion year interval for each panel with 100 million-year time steps (coloured lines). The black dots on the right edge of the panels show the position of the GCs at the beginning for each set of a billion years. The black lines represent the values of the gravitational potential for each Oort particle due to only the Sun for the FIX and 411321 potentials. This gravitational potential from the Sun can be described as a simple function ∼R⁻¹. For the potential normalisation, we used the N-body units of global integration: G = 1, MU = 2.325 ⋅ 10⁹ M_⊙, RU = 1 kpc, VU = 100 km/s.

Fig. C.1. Values of the gravitational potential (with ’-’ sign) for each Oort particle in FIX and 411321 potentials for the first three billion years. Black lines are particle potentials without the GC influence, and colour lines are the same but with the GC influence. Each panel represents one billion years in look-back time integration. The FIX potential is presented in the left panels, and 411321 is on the right panels.

Fig. C.2. Same as in Fig. C.1 but for the 3–6 Gyr interval.

The coloured lines represent the distribution of the Oort particles in the FIX and 411321 potentials due to the gravitational influence of the GCs. In these cases, the influence of the GCs on the Oort system is more complex and has a pronounced flat part in outer radii, R > 2 pc. In the right panels, we observed that the influence of the GCs in the case of 411321 TNG-TVP is stronger, and many more stripped former Oort particles become bound with the flyby GCs. In a late phase of the evaluation (after ∼3 Gyr), we observed a strong separation between the different families of the Oort particle orbits. The gap formation at the R = 2 pc is directly connected with the process of the Oort cloud particles’ strong tidal stripping due to the direct gravitational influence of the GCs. The captured particles at R > 1 kpc are under the strong gravitational influence of the GCs. In this case, their gravitational potential is no longer connected with the Sun but is mainly defined by the influence of the closest GC.

All Tables

All Figures

Fig. 1. Average probability of the number of passages (left panel) between GCs and SolS as a function of the relative distance dR. The black dashed lines are the linear fit for the corresponding potentials. The right panel presents the average probability of the cumulative number of passages as a function of the minimum relative distance dR of the GCs at the moment of closest approach in all six potentials. Colours: 411321 – red, 441327 – green, 451323 – blue, 462077 – magenta, and 474170 – cyan. The brown colour is for the FIX potentials.

In the text

	Fig. 2. Relative velocities (left panel) and time when close passages happen (right panel) between the GCs and the SolS. Colours: 411321 – red, 441327 – green, 451323 – blue, 462077 – magenta, and 474170 – cyan. The brown colour is for the FIX potentials.
In the text

Fig. 3. Oort particle distributions due to gravitational influence of GCs. The different zones are as follows: Less than 2 pc – inner zone (top panel), from 2 pc to 1000 pc – middle zone (middle panel), and above 1000 pc – outer zone (bottom panel). The solid lines show the particle distribution, and dotted lines show moments of the GC deep passages. The colours represent potentials. The larger green dots represent the results with the N = 50 k Oort cloud number (re-scaled).

In the text

Fig. B.1. Orbital Sun evolution with close passages during the whole integration time in 411321 TNG-TVP. Coloured circles: green for BH 140, red for UKS 1, blue for Djorg 1, magenta for NGC 7078, cyan for NGC 2808. The hollow circles outlined in grey are other GCs. The blue point is the start of integration. From top to bottom, the panels represent the interval of integration: 0 – 2 Gyr, 2 – 4 Gyr, and 4 – 6 Gyr in look-back time.

In the text

Fig. C.1. Values of the gravitational potential (with ’-’ sign) for each Oort particle in FIX and 411321 potentials for the first three billion years. Black lines are particle potentials without the GC influence, and colour lines are the same but with the GC influence. Each panel represents one billion years in look-back time integration. The FIX potential is presented in the left panels, and 411321 is on the right panels.

In the text

	Fig. C.2. Same as in Fig. C.1 but for the 3–6 Gyr interval.
In the text