The food was excellent. The bar downstairs was fantastic. We will come back. Monaco will always be a gem to discover! So much to see and do, even in November. The hotel is great. The view from first floor is wonderful- we could see all the yachts and the palace and the sea. What to say about the staff more then they were very nice. Add a complete breakfast, a Michelin restaurant and a spa and yuhuuuu, you got your perfect weekend destination! Superb service, luxuriously renovated, very good breakfast, spacious room.
My husband said that it was the best hotel we ever stayed so far. And we have stayed in soooo many hotels usually 4 or 5 stars. We loved everything about it, great hotel, great location, huge rooms and all the rest is just fantastic. List your property.
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Choose your dates to see up-to-date prices and availability. I'm traveling for work. All 5-star hotels 5-Star Hotels Apartments. Monaco 5-Star Hotels Hotels. Monte Carlo. Monte Carlo — 3 five-star hotels found. Show more Show less. Check availability. Everything was great, the room itself was OK Show more Show less. It features a winter garden and guests can access the 7, m2 spa. A minibar, flat-screen TV and period furnishings feature in the individually decorated and air-conditioned rooms at H?
Each room has a view of the city, garden or the sea. A DVD player and video games are available upon request. A selection of vintage wines and spirits are served in the Crystal Bar, with its leather armchairs.
You can request seawater treatments and enjoy a sauna session, and the fitness centre offers a panoramic sea view. Free WiFi is available in the hotel lobby. Nice Airport is a minute drive from the hotel and a helicopter service is possible upon request. Free shuttles are provided for access to the private beach. Hotel Metropole, Monte Carlo. Excellent 12 Reviews. RoomsMake yourself at home in one of the air-conditioned rooms featuring minibars and flat-screen televisions.
Your pillowtop bed comes with down comforters and Egyptian cotton sheets. Complimentary wireless Internet access keeps you connected, and satellite programming is available for your entertainment. Rec, Spa, Premium AmenitiesRelax at the full-service spa, where you can enjoy massages, body treatments, and facials.
If you're looking for recreational opportunities, you'll find an outdoor pool, a sauna, and a steam room. From your room, you can also access hour room service.
Buffet breakfasts are available daily for a fee. Planning an event in Monaco? This hotel has square feet square meters of space consisting of conference space and meeting rooms. A roundtrip airport shuttle is provided for a surcharge available on request. You must present a photo ID when checking in. Your credit card is charged at the time you book. Bed type and smoking preferences are not guaranteed.
Your reservation is prepaid and is guaranteed for late arrival. The total charge includes all room charges. Special Discount. Fairmont Monte Carlo. Excellent 16 Reviews. This impressive hotel complex enjoys a prime setting in Monte Carlo, overlooking the shimmering waters of the Mediterranean Sea. The hotel is located just a short distance away from the casino and a shopping centre. The opera house and the theatre are just a short walking distance away, while links to the public transport network are to be found just metres from the hotel.
This wonderful hotel lies just a 10 minutes' walking distance from Monaco Monte train station. This wonderful hotel welcomes guests into a world of luxury and splendour. The guest rooms are sumptuously appointed, bathing visitors in luxury and style.
The hotel features a seemingly boundless array of first-class facilities, meeting the leisure, dining, business and recreational needs of every type of traveller to a high level of excellence. Novotel Monte-Carlo. RoomsMake yourself at home in one of the air-conditioned rooms featuring flat-screen televisions.
Private bathrooms with separate bathtubs and showers feature complimentary toiletries and hair dryers. Conveniences include safes and desks, and housekeeping is provided daily.
Rec, Spa, Premium AmenitiesTake advantage of recreational opportunities offered, including an outdoor pool, a steam room, and a fitness center.
DiningGrab a bite to eat at the hotel's restaurant, where you can take in a garden view, or stay in and take advantage of room service during limited hours. Event facilities at this hotel consist of conference space and meeting rooms. Self parking subject to charges is available onsite. The total charge includes all room charges and taxes, as well as fees for access and booking. Any incidental charges such as parking, phone calls, and room service will be handled dir.
Outstanding 18 Reviews. RoomsMake yourself at home in one of the air-conditioned rooms featuring minibars. Cable programming provides entertainment, and wired and wireless Internet access is available for a surcharge. Private bathrooms have complimentary toiletries and hair dryers. Rec, Spa, Premium AmenitiesRelax on the private beach or enjoy other recreational amenities such as a health club and an indoor pool. DiningTake advantage of the hotel's hour room service. A roundtrip airport shuttle is available for a surcharge.
Any incidental charges such as parking, phone calls, and room service will be handled directly between you and the property.
Outstanding 11 Reviews. Located in Monaco, this elegant hotel offers guest rooms with free Wi-Fi access and a minibar. All air-conditioned guest rooms are equipped with a TV with cable channels. Some rooms at the Ambassador-Monaco feature a seating area. Each guest room has floor-to-ceiling windows offering plenty of natural light. Ambassador-Monaco features a pizzeria serving traditional Italian cuisine.
Guests can enjoy a drink in the hotel bar. A buffet breakfast is served every morning. However, this is not the case. It seems that the initial strong mass loss in BM dominates the later mass loss due to tidal stripping, setting from the very beginning large tangential anisotropy.
Nevertheless, the main features of fig. Three main effects may be expected to govern the evolution of the mass function in models studied in this paper. First, there is a period of violent mass loss due to sellar evolution of the most-massive stars. It takes place mainly during the first few hundred million years and its amplitude strongly depends on the slope of the mass function.
Secondly, there is the process of rapid mass segregation, caused by two-body distant encounters relaxation. It takes place mainly during core collapse and is relatively unaffected by the presence of a tidal field. Thirdly, there is the effect of the tidal field itself, which becomes more important after core collapse or even earlier for models with a shallow mass function and with low concentration.
Because the tides preferentially remove stars from the outer parts of the system, which are mainly populated by low-mass stars mass segregation , one can expect that the mean mass should increase as evolution proceeds, making allowance for stellar evolution. The basic results are illustrated in Fig. The violent and strong mass loss due to stellar evolution is characterized by an initial decrease in the mean mass.
The evolution of the most-massive stars will remove a substantial amount of mass from the system and, consequently, only slightly lower the mean mass in the whole system. This behaviour is visible also in the other models, but with one exception. The mean mass inside the 10 per cent Lagrangian radius for model W increases instead of decreasing.
For this model, the initial concentration is high enough to force very quick mass segregation in the central part of the system. The most-massive unevolved main-sequence stars, white dwarfs and neutron stars, sink into the centre.
For model W, for most of the time the mean mass stays nearly constant for the whole system. Just before the cluster dissolution, it substantially increases. For all models, tidal stripping connected mainly with removal of less-massive stars forces the mean mass in the middle and outer parts of the system to steadily increase. The much faster increase in the mean mass inside the 10 per cent Lagrangian radius mass segregation than that in the outer Lagrangian radii 50 and 99 per cent during the collapse phase nearly stops at the core bounce time.
The subsequent evolution is characterized by the slower rate of increase in the mean mass close to the time of the core bounce, the mean mass is practically constant. The reason for the nearly constant mean mass is unclear. The slow increase in the mean mass can be attributed to the binary activity, which leads to removal of some low-mass stars from the core.
For all models, the effect of tides manifests itself by a gradual increase in the mean mass in the halo. The evolution of the mean mass for main-sequence stars and white dwarfs for the inner 10 per cent Lagrangian radius is shown in Fig. When less and less massive main-sequence stars finish their evolution as less and less massive white dwarfs, the mean mass of white dwarfs decreases with time.
The newly created less-massive white dwarfs affect the mean mass of white dwarfs more strongly for the steeper mass function than for the shallower mass function. For the steeper mass function, a smaller number of massive white dwarfs are created comparable to the shallower mass function. At the time around the core bounce, the mean mass of white dwarfs increases. This is connected with the decreasing core size and continuing mass segregation.
Deeper in the cluster centre, a higher fraction of massive white dwarfs are present. In the post-collapse phase, the white dwarfs' mean mass decreases.
Binaries start to be created mainly from the most-massive stars neutron stars and white dwarfs deep in the core. They dynamically interact with other stars and in the course of evolution are removed from the system together with some massive white dwarfs. This leads to the decrease in the mean mass of white dwarfs. The mean mass of main-sequence stars, inside 10 per cent Lagrangian radius, initially slightly decreases, which is connected with stellar evolution of the most-massive stars.
There is then a period of gradual increase in the mean mass due to mass segregation. At late phases of cluster evolution, the rate of increase in the mean mass speeds up.
Around the core bounce time, one can observe break in the rate of increase in the main-sequence mean mass. This can be again attributed to binary activities. The evolution of the total mean stellar mass in the different regions of the system Fig.
Stellar evolution will change the stellar content of the cluster. In the course of time, main-sequence stars will evolve, creating first black holes, neutron stars and then white dwarfs with decreasing masses. In Fig. The fraction of evolved stars present in the system at any time result from two processes which act in opposite directions: stellar evolution formation and evaporation across the tidal boundary loss.
At the beginning of cluster evolution, the sharp increase in the mass ratio of evolved stars and the decrease in the mass ratio of main-sequence stars and the total mass ratio are connected with the stellar evolution of the most-massive stars in the system. The steady increase in the mass ratio for wd and ns is then observed. After the time of core bounce, the ratio for ns slowly decreases because of binary activities [the most-massive stars neutron stars have the highest probability of being involved in binary formation and of being finally removed from the system by interactions with the field stars and other binaries].
At time close to the dissolution time, evolved stars consist of up to 75 per cent of the mass of all stars and up to 63 per cent of the number of all stars.
This is in a very good agreement with the results obtained by VH and BM. It is worth noting that systems at the time of dissolution still consist of a substantial number of unevolved low- and very low-mass main-sequence stars.
So, the mass and number fractions of evolved stars can be very large but cannot approach per cent. As expected, the mass-segregation process and removal of less-massive stars due to the evaporation process across the tidal boundary cause a steady increase in the mass ratios.
For the inner part of the system up to about the 5 per cent Lagrangian radius , during the core-collapse time, the rate of increase in the mass ratio is the fastest anywhere in the system. However, after core bounce, the rate there becomes the slowest and the mass ratio of evolved stars is nearly constant. This is connected with the fact that the mass-segregation process is nearly completed at the time of core bounce see Fig.
The further slight increase in the mass ratio can be mainly attributed to binary activity. For parts of the system outside the 10 per cent Lagrangian radius, the behaviour of the mass ratio is opposite to that discussed earlier.
During the collapse phase, the rate of increase in mass ratio is slower than that in the post-collapse phase. This behaviour can be attributed to the properties of the stripping process, which is more and more effective when deeper and deeper parts of the system are exposed.
In between these two zones Lagrangian radius between 5 and 10 per cent , the rate of increase in mass ratio is nearly constant during the whole evolution. The amount of mass in evolved stars in the core can be as high as 97 per cent and in the outer parts of the system up to 65 per cent, at a time close to the dissolution time.
The same qualitative behaviour is observed for other models. However, for models with a steeper IMF and for more-concentrated models, the mass ratios are smaller. For initially more-concentrated models, the time of core bounce is much shorter than for the less-concentrated models.
So, the process of mass segregation is less advanced and therefore the mass ratios are smaller. Also, for more-concentrated cluster W , the evaporation process is less effective. The ratios are about 10 per cent smaller than those for W model. For the model W, which does not enter the post-collapse evolution before cluster dissolution, the mass ratios behave like those for other models in the collapse phase, but the spread between ratios in different zones is much smaller.
It is worth noting that a cluster at the time 15 Gyr can consist of up to 90 per cent of evolved stars in the core and up to 10 per cent of evolved stars in the outer parts of the system.
This conclusion has very important observational consequences. The presence of a substantial number of practically invisible stars has to be taken into account when the global globular cluster parameters are drawn from the observations.
Evolution of the ratio of evolved stars to the actual total mass for different zones: R 0—0. The mass loss connected with the stellar evolution of those stars and tidal stripping induced by it will strongly reduce the cluster mass and the number of bound stars. This will lead to a substantial decrease in the half-mass relaxation time and consequently to a sped-up cluster evolution. For systems initially not strongly bound, this can even lead to quick dissolution, which would not happen otherwise.
Additionally, the presence of a larger number of massive compact remnants white dwarfs, neutron stars and black holes , comparable to systems with a lower maximum stellar mass, will increase because of mass segregation mean mass and remnant fraction in the central parts of the system.
These conclusions are in good agreement with results obtained by BM. The mean mass in their simulations is larger than for simulations presented in this paper. This leads to substantially larger mean mass and remnant fraction in the central part of the system.
According to VH, the mass slope of a mass function can be obtained from the numerical data in the following way:. According to VH, m 1 and m 2 were chosen to be 0. The LMF was calculated for three zones VH : up to 30 per cent Lagrangian radius, between 30 and 60 per cent Lagrangian radii and from 60 per cent Lagrangian radius up to the tidal radius.
In the case when only mass segregation is taken into account, the LMF in the inner parts of the system becomes flatter and in the outer parts becomes steeper. The evaporation process acts in the opposite direction. It tends to flatten the mass function because of the preferential removal from the system particularly from the outer parts of low-mass stars.
For all the discussed models, the LMF for the outermost parts of the system initially increases. The increase is slightly higher for more-concentrated systems with the same IMF this is consistent with the picture of mass segregation , and even more pronounced for the system with the same concentration but with steeper mass function.
The IMF during dynamical cluster evolution is very quickly forgotten and practically impossible to recover from the observational data. The actual GMF of globular clusters can be recovered from observational data for the middle parts of the system close to the half-mass radius.
The results discussed above are in a very good agreement with the results obtained by VH for N -body runs.
Evolution of the power-law index of the mass function for different shells: R 0—30 , R 30—60 , R 60— r t and for the GMF for model W The power-law index was computed for main-sequence stars in the mass range 0. This paper is a continuation of Paper I and II, in which it was shown that the Monte Carlo method is a robust scheme to study, in an effective way, the evolution of very large N -body systems.
The Monte Carlo method describes in a proper way the graininess of the gravitational field and the stochasticity of real N -body systems. It provides, in almost as much detail as N -body simulations, information about the movement of any object in the system. In that respect, the Monte Carlo scheme can be regarded as a method which lies between direct N -body and Fokker—Planck models and combines most advantages of both methods.
This is the first important step in the direction of simulating the evolution of a real globular cluster. Particularly good agreement is obtained with VH's N -body simulations and, not surprisingly, with the results of Monte Carlo simulations presented in Paper II. All models survive the phase of rapid mass loss and then undergo core collapse and then subsequent post-collapse expansion except model W in a manner similar to isolated models.
The expansion phase is eventually reversed when tidal limitation becomes important. As in isolated models, mass segregation substantially slows down by the end of core collapse. During this phase of evolution, the rate of mass loss is nearly constant, and higher for shallower mass functions. The development of a power-law density profile is clearly visible.
This value is close to the theoretically predicted value for the most-massive component CW, see equation The strongly concentrated model W , shows a modest initial build-up of anisotropy in the outer parts of the system. As tidal stripping exposes the inner parts of the system, the anisotropy gradually decreases and eventually becomes slightly negative.
Model W from the very beginning develops negative anisotropy in the outer parts of the system. The cluster is not concentrated enough to prevent removal of stars which are preferentially on radial orbits. The anisotropy stays negative until the time of cluster disruption, when it becomes slightly positive during cluster disruption, most stars are on radial orbits. Because of mass segregation, and due to evaporation across the tidal boundary, which preferentially removes low-mass stars, the mean mass in the cluster increases with time.
During the core collapse, the rate of increase in the mean mass is highest in the central parts of the system mass segregation. After the core bounce, there is a substantial increase in the mean mass in the middle and outer parts of the system tidal stripping , and a more modest increase in the inner parts of the system, which is mainly connected with binary activity.
The fraction of evolved stars increases during the cluster evolution. This fraction is larger for systems with shorter relaxation time and stronger influence of the tidal field of a parent galaxy. The mass ratio of evolved stars can be as high as nearly 65 per cent in the outer parts of the system and up to nearly 98 per cent in the core.
At the time of 15 Gyr, these ratios are 90 and 10 per cent, respectively. The presence of a substantial number of practically invisible stars has very important consequences for the interpretation of observational data and it has to be taken into account when the global globular cluster parameters are drawn from the observations. Because of stellar evolution, mass segregation and evaporation of stars, the IMF is quickly forgotten and impossible to recover from the observational data.
These results are in an excellent agreement with N -body simulations presented by VH. In order to perform simulations of real globular clusters, the description of some processes already included in the code has to be improved, and several additional physical processes have to be added to the code. Stellar and binary evolutions, more accurate treatment for energy generation by binaries, particularly in binary—binary interaction, and proper treatment of the escape process in the presence of a tidal field are still waiting for improvement.
One of the population-synthesis codes developed by Hurley Hurley et al. The treatment of escapers proposed by Spurzem et al. The tidal shock heating of the cluster due to passages through the Galactic disc, interaction with the bulge, shock-induced relaxation, primordial binaries, physical collisions between single stars and binaries are some of the processes which are waiting for implementation into the code. The inclusion of all these processes does not pose a fundamental theoretical challenge, but is rather complicated from the technical point of view.
Inclusion into the Monte Carlo code of as many physical processes as possible will allow us to perform detailed comparison between simulations and observed properties of globular clusters, and will also help us to understand the conditions of globular cluster formation and explain how peculiar objects observed in clusters can be formed. These types of simulations will also help us to introduce, in a proper way, into future N -body simulations all the necessary processes required to simulate the evolution of real globular clusters on a star-by-star basis from their birth to their death.
I would like to thank Douglas C. Heggie and Rainer Spurzem for stimulating discussions, comments and suggestions.
Aarseth S. Heggie D. Baumgardt H. Fuchs B. Just A. Spurzem R. Wielen R. Google Scholar. Google Preview. Makino J. Hut P. Taam R.
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