Tourism in Dubai is a major part of the economy of Dubai. Dubai was the third most visited city in the world in 2023 with 17 million international visitors according to Euromonitor International.[1][2] Dubai hosts more than 800 hotels with more than 150,000 rooms.[3][4]
The discovery of oil in 1966 kick-started the development of present Dubai, however Sheikh Hamad bin Maktoum (ruler from 1958 till 1990) realised one day Dubai would run out of oil and started building an economy that would outlast it.[5] A quote commonly attributed to Sheikh Rashid reflected his concern that Dubai's oil, which was discovered in 1966 and which began production in 1969, would run out within a few generations. Sheikh Rashid stated "My grandfather rode a camel, my father rode a camel, I drive a Mercedes, my son drives a Land Rover, his son will drive a Land Rover, but his son will ride a camel".[6] Sheikh Rashid realized early he needed to diversify the emirate of Dubai's economy by building on the city's trading history and therefore he set out to establish Dubai as the region's trade and service hub. By 1979, he was successful in establishing the Jebel Ali Port, which became the logical shipping centre for the entire United Arab Emirates and the world's largest man-made port. He also upgraded Dubai International Airport and built the Dubai World Trade Centre, which was then the tallest building in the Middle East. By the end of the 1970s, the stage was set for the diversification of Dubai's economy away from oil and into other areas such as tourism.[7]
In 1989 the Dubai Commerce and Tourism Promotion Board was established, to promote Dubai as a luxury destination for the up-tier market and influential business sectors. In January 1997, it was replaced with the Department of Tourism and Commerce Marketing (DTCM).[8]
In May 2013, the government of Dubai launched the Dubai Tourism Strategy 2020, with the key objective to attract 20 million visitors a year by 2020 and making Dubai a first choice destination for international leisure travellers as well as business travellers.[9] In 2018, the strategy was expanded by setting new goals of attracting 21-23 million visitors in 2022 and 23-25 million visitors by 2025.[10] The key objectives from 2013 and 2018 were not met due to the COVID-19 pandemic.
The need to maintain its tourism industry has hampered Dubai's response to the COVID-19 pandemic.[11] Along with COVID-19 Dubai's tourism sector has also been hurt by a greater international awareness of the status of human rights in the emirate and in particular the treatment of Princess Latifa bint Mohammed Al Maktoum.[12]
In November 2022, Sheikh Mohammed bin Rashid announced a national tourism strategy until 2031. The goal of the strategy is to attract Dh 100 billion in additional tourism investments (so that the tourism sector's contribution will be Dh450bn of Dubai's GDP in 2031) and receive 40 million hotel guests in 2031. The strategy includes 25 initiatives and policies to support the development of the tourism sector in the country.[13]
In April 2025, the Dubai Department of Economy and Tourism introduced a new programme offering media training to students for promotion of tourism in the UAE. Applicants are provided with flights, luxury apartment and three months of income, along with certification from Dubai College of Tourism for posting about traveling experiences in Dubai on social media. According to Middle East Eye, this program aims to whitewash its human rights violations and war crime accusations in Sudan.[14]
Since 1982, Dubai continued to be one of the fastest growing destinations for tourists. In 2002, visitors were mainly from other Gulf Cooperation Council members which accounted for 34% of tourists, South Asia accounted for 25%, other Arab states 16%, Europe 15%, and Africa 9%. In 2003, revenue from tourism exceeded $1 billion and surpassed oil revenues to directly and indirectly account for over 17% and 28% of GDP respectively.[15]
From January to June 2019 8.36 million international tourists visited Dubai. Most of the visitors were from India (997,000) followed by Saudi Arabia (755,000) and the United Kingdom (586,000).[16]
Mastercard's Global Destination Cities Index 2019 found that tourists spend more in Dubai than in any other country. In 2018, the country topped the list for the fourth year in a row with a total spend of $30.82 billion, a 3.8% increase over 2017 ($29.70 billion). The average spend per day was $553.[17]
In 2019, Dubai attracted a total of 16.73 million tourists, which was an increase of 5.09% on the previous year. However, in 2020, the number of visitors dropped to 5.51 million due to the coronavirus pandemic.[18]
| Year | Total international visitors [19][20][21][15][22][23] |
Increase/decrease | Visitor spending ($m)[24] |
|---|---|---|---|
| 1982 | 374,400 | N/a | |
| 1990 | 632,903 | ||
| 1991 | 716,642 | ||
| 1992 | 944,350 | ||
| 1993 | 1,088,000 | ||
| 1994 | 1,239,000 | ||
| 1995 | 1,601,000 | 632.0 | |
| 1996 | 1,768,000 | 743.0 | |
| 1997 | 1,792,000 | 814.0 | |
| 1998 | 2,184,000 | 859.0 | |
| 1999 | 2,481,000 | 893.0 | |
| 2000 | 3,027,000 | 1,063.0 | |
| 2001 | 3,626,625 | 1,200.0 | |
| 2002 | 4,756,280 | 1,332.0 | |
| 2003 | 4,980,228 | 1,438.0 | |
| 2004 | 5,420,000 | 1,593.0 | |
| 2005 | 6,160,003 | 3,218.0 | |
| 2006 | 6,441,670 | 4,972.0 | |
| 2007 | 6,951,798[25][26] | 6,072.0 | |
| 2008 | 6,996,449[25] | 7,162.0 | |
| 2009 | 7,580,000[27] | 7,352.0 | |
| 2010 | 8,410,000 | 8,577.0 | |
| 2011 | 9,910,000 | 9,204.0 | |
| 2012 | 10,950,000 | 10,924.0 | |
| 2013 | 12,900,000 | 12,389.0 | |
| 2014 | 13,200,000 | 15,221.0 | |
| 2015 | 14,200,000 | 25,587.1 | |
| 2016 | 14,870,000 | 28,657.4 | |
| 2017 | 15,790,000 | 29,705.5 | |
| 2018 | 15,920,000 | 34,609.5 | |
| 2019 | 16,730,000 | 38,413.3 | |
| 2020 | 5,510,000[a] | 24,615.4 | |
| 2021 | 7,280,000[b] | ||
| 2022 | 14,360,000[28] | ||
| 2023 | 17,150,000[29] | ||
| 2024 | 18,720,000[30] |
In the last three years, Dubai saw an increase in 4 and 5 star hotels and number of rooms, but a decrease in standard hotel apartments. The total number of rooms increased by 9,098 from 2015 to 2017, an increase of 9.25%. Prior to the Expo 2020 hotels in Dubai were reducing room rates to stimulate demand as supply accelerated. Based on data of August 2019, Dubai hoteliers reported a 7.6% rise in supply against 7.4% increase in demand.[31] Average room rates stood at AED 486 in June 2019 while in the same month of 2018 average room rates were at 544 AED.[32] In July 2019, Dubai's Jumeirah Group LLC fired 500 people due to a decline in tourism. In the second quarter of 2019, hospitality sector has had the worst quarter since 2009.[33]
| 2014 | 2015 | 2016 | 2017 | 2018 | 2019 | 2020 | 2021 | 2022 | 2023 | |
|---|---|---|---|---|---|---|---|---|---|---|
| Total 5 star hotels | 91 | 96 | 103 | 113 | 128 | 134 | 143 | 151 | 157 | |
| Total 5 star hotel rooms | 31,551 | 33,122 | 35,853 | 38,543 | 43,133 | 44,067 | 47,035 | 49,585 | 51,809 | |
| Total 4 star hotels | 106 | 112 | 122 | 146 | 158 | 161 | 181 | 189 | 194 | |
| Total 4 star hotel rooms | 21,208 | 22,990 | 25,289 | 29,908 | 33,120 | 34,905 | 40,377 | 42,505 | 43,283 | |
| Total 1-3 star hotels | 264 | 267 | 260 | 260 | 258 | 225 | 243 | 270 | 274 | |
| Total 1-3 star hotel rooms | 19,714 | 21,767 | 21,591 | 22,634 | 24,491 | 21,732 | 25,384 | 28,512 | 28,789 | |
| Total hotel apartments (deluxe/superior) | 66 | 66 | 65 | 68 | 68 | 74 | 80 | 82 | 85 | |
| Total deluxe/superior rooms | 9,641 | 9,519 | 9,786 | 10,522 | 10,520 | 11,845 | 12,606 | 13,113 | 13,842 | |
| Total hotel apartments (standard) | 150 | 140 | 131 | 129 | 129 | 117 | 108 | 112 | 111 | |
| Total standard rooms | 16,219 | 15,447 | 14,930 | 14,360 | 14,856 | 14,398 | 12,548 | 12,781 | 12,568 | |
| Total establishments | 657 | 677 | 681 | 681 | 716 | 741 | 711 | 755 | 804 | 821 |
| Total available rooms | 92,333 | 98,333 | 102,845 | 107,431 | 115,967 | 126,120 | 126,947 | 137,950 | 146,496 | 150,291 |
| Average occupancy | 79% | 77% | 78% | 78% | 76% | 75% | 54% | 67% | 73% | 77% |
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| Rank | Country | 6/2023 | 2022 |
|---|---|---|---|
| 1 | 1,223,000 | 1,842,000 | |
| 5 | 616,000 | 758,000 | |
| 4 | 555,000 | 1,043,000 | |
| 3 | 538,000 | 1,216,000 | |
| 2 | 511,000 | 1,311,000 | |
| 6 | 362,000 | 590,000 | |
| 7 | 329,000 | 422,000 | |
| 17 | 260,000 | 177,000 | |
| 10 | 196,000 | 328,000 | |
| 13 | 196,000 | 239,000 | |
| 8 | 180,000 | 364,000 | |
| 11 | 168,000 | 288,000 | |
| 12 | 152,000 | 260,000 | |
| 9 | 152,000 | 356,000 | |
| 14 | 145,000 | 234,000 | |
| 15 | 130,000 | 212,000 | |
| 19 | 125,000 | 158,000 | |
| 16 | 121,000 | 184,000 | |
| 18 | 110,000 | 158,000 | |
| 19 | 110,000 | 148,000 |
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Aspects of Dubai's old culture, while occasionally overshadowed by the boom in economic development, can be found by visiting places around the creek, which splits Dubai into two halves, Bur Dubai and Deira. The buildings lining the Bur Dubai side of the Creek provide the main flavor of the old city. Heritage Village is one of the few remaining parts of historical Dubai, containing preserved buildings. The adjoining Diving Village offers exhibits on pearl diving and fishing. The Diving Village forms part of an ambitious plan to turn the entire "Shindagha" area into a cultural city, recreating life in Dubai as it was in days gone by.
Other attractions include the Sheikh Saeed Al Maktoum House; the Dubai Museum in the restored Al Fahidi Fort, which was erected around 1799; and the Heritage Village of Hatta, situated 115 kilometers southeast of Dubai City in the heart of the rocky Hatta Mountains. The history of the village can be traced back 2000 – 3000 years. It consists of 30 buildings, each differing in size, interior layout and building materials used. Great care was taken to use the same materials as those used when originally built during the renovation such as mud, hay, sandalwood and palm fronds. The Sharia Mosque is an old mosque built in the early 19th century using the same building materials and consists of a large prayer hall, a court and courtyard, minaret and other utility rooms.[34] Other museums include the Al Ahmadiya School.
Dubai has been nicknamed the "shopping capital of the Middle East."[35][36] The city draws large numbers of shopping tourists from countries within the region and from as far as Eastern Europe, Africa and the Indian Subcontinent. Dubai is known for its souk districts. Souk is the Arabic word for market or place where any kind of goods are brought or exchanged. Traditionally, dhows from the Far East, China, Sri Lanka, and India would discharge their cargo and the goods would be bargained over in the souks adjacent to the docks.[37]
Modern shopping malls and boutiques are also found in the city. Dubai Duty Free at Dubai International Airport offers merchandise catering to the multinational passengers using Dubai International Airport. Outside of Duty Free areas and major sales, Dubai has a reputation for being one of the most expensive shopping destinations in the world.[38]
While boutiques, some electronics shops, department stores and supermarkets may operate on a fixed-price basis, most other outlets consider friendly negotiation as a way of life.
Dubai's numerous shopping centres cater for every consumer's need. Cars, clothing, jewellery, electronics, furnishing, sporting equipment and any other goods will all be likely to be under the same roof.[39]
The Dubai Shopping Festival is a month-long festival held during the month of January each year. During the festival the entire emirate becomes one massive shopping mall. Additionally, the festival brings together music shows, art exhibitions, and folk dances.[40]
The Dubai Summer Surprises (DSS) is the summer version of Dubai Shopping Festival held during June, July and August. Dubai Government launched Dubai Summer Surprises in 1998 in order to promote Dubai as a family holiday destination. DSS offers fun, entertainment, food deals and great offers on shopping.
Tourists are required to obey some Muslim religious restrictions in public even if they are not Muslim themselves, such as refraining from eating or drinking in public places in the daytime during Ramadan.[41]
Dubai has a modest dress code as part of its criminal law.[42] Sleeveless tops and short dresses are not encouraged at Dubai Mall.[43][44] Clothes are advised to be in appropriate lengths.[42]
Homosexuality is criminalized in Dubai, including for tourists. However, there is a vibrant underground gay scene in Dubai and authorities do not actively search for homosexuals to enforce the law.[45]
Most capitals and other major cities have direct flights to Dubai. More than 120 airlines operate to and from Dubai International Airport to more than 260 destinations. Dubai International Airport is the world's busiest airport by international passenger traffic.[46] Dubai is also the home base of the airline Emirates, which operates scheduled services to more than 100 destinations.
In June 2009 Emirates designated a special handling area at departures and arrivals for passengers with special needs, allowing wheelchair passengers to receive a more personalized service.[47][better source needed]
The establishment of the first cruise terminal in Dubai in 2001 and the opening of the enhanced New Dubai Cruise Terminal in February 2010 with higher handling capacity has drawn the attention of cruise line operators. Cruises to Dubai sail from: Singapore, Sydney, Athens, Dover, Venice, Cape Town, Civitavecchia, Piraeus, Alexandria, Istanbul, New York City, Southampton, Barcelona, Fort Lauderdale, Miami, Los Angeles, Mumbai, Hong Kong, Shanghai, Monte Carlo, Mombasa, Victoria, and Cairns among others.[48][better source needed]
The United Arab Emirates has a network of roads that connect major towns and villages, including a multi-lane highway between Dubai and Abu Dhabi, with access to and from the bordering countries of Saudi Arabia and Oman. Highways and main roads in Dubai and the United Arab Emirates are designated by an Emirate Route Number. Speed limits are displayed on road signs and are usually 60–80 km/h (37–50 mph) around town and 100–120 km/h (62–75 mph) elsewhere.[49][better source needed]
Dubai ranked third in the best taxi services behind Tokyo and Singapore.[50][better source needed]
Travelers entering Dubai are warned for harsh penalties regarding illicit drug use or smuggling. Authorities in Dubai use highly sensitive equipment to conduct thorough searches to find trace amount of illegal substances.[51] A senior Dubai judge was quoted on February 11, 2008, by the Dubai City News saying, "These laws help discourage anyone from carrying or using drugs. Even if the quantity of illegal drugs found on someone is 0.05 grams, they will be found guilty. The penalty is a minimum of four years. The message is clear — drugs will not be tolerated."[51]
No special immunizations are required, but tourists are encouraged to purchase appropriate medical insurance before travelling. Government immunization programs have led to recognition by a travel magazine.[47] As a latest addition to the established modern health care system, Dubai offers online health care contacts of virtually all medical doctors in Dubai.[52]
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Dubai hosts the following international championships:
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|
| Observation data Epoch J2000 Equinox J2000 |
|
|---|---|
| Constellation | Ursa Minor |
| Pronunciation | /pəˈlɛərɪs, -ˈlær-/; UK: /pəˈlɑːrɪs/[1] |
| α UMi A | |
| Right ascension | 02h 31m 49.09s[2] |
| Declination | +89° 15′ 50.8″[2] |
| Apparent magnitude (V) | 1.98[3] (1.86 – 2.13)[4] |
| α UMi B | |
| Right ascension | 02h 30m 41.63s[5] |
| Declination | +89° 15′ 38.1″[5] |
| Apparent magnitude (V) | 8.7[3] |
| Characteristics | |
| α UMi A | |
| Spectral type | F7Ib + F6V[6] |
| U−B color index | 0.38[3] |
| B−V color index | 0.60[3] |
| Variable type | Classical Cepheid[4] |
| α UMi B | |
| Spectral type | F3V[3] |
| U−B color index | 0.01[7] |
| B−V color index | 0.42[7] |
| Variable type | suspected[4] |
| Astrometry | |
| Radial velocity (Rv) | −17[8] km/s |
| Proper motion (μ) | RA: 44.48±0.11[2] mas/yr Dec.: −11.85±0.13[2] mas/yr |
| Parallax (π) | 7.54±0.11 mas[2] |
| Distance | 446.5±1.1 ly (136.90±0.34 pc)[9] |
| Absolute magnitude (MV) | −3.6 (α UMi Aa)[3] 3.6 (α UMi Ab)[3] 3.1 (α UMi B)[3] |
| Position (relative to α UMi Aa) | |
| Component | α UMi Ab |
| Epoch of observation | 2005.5880 |
| Angular distance | 0.172″ |
| Position angle | 231.4° |
| Position (relative to α UMi Aa) | |
| Component | α UMi B |
| Epoch of observation | 2005.5880 |
| Angular distance | 18.217″ |
| Position angle | 230.540° |
| Orbit[9] | |
| Primary | α UMi Aa |
| Companion | α UMi Ab |
| Period (P) | 29.416±0.028 yr |
| Semi-major axis (a) | 0.12955±0.00205" (≥2.90±0.03 AU[10]) |
| Eccentricity (e) | 0.6354±0.0066 |
| Inclination (i) | 127.57±1.22° |
| Longitude of the node (Ω) | 201.28±1.18° |
| Periastron epoch (T) | 2016.831±0.044 |
| Argument of periastron (ω) (primary) |
304.54±0.84° |
| Semi-amplitude (K1) (primary) |
3.762±0.025 km/s |
| Details | |
| α UMi Aa | |
| Mass | 5.13±0.28[9] M☉ |
| Radius | 46.27±0.42[9] R☉ |
| Luminosity (bolometric) | 1,260[11] L☉ |
| Surface gravity (log g) | 2.2[12] cgs |
| Temperature | 6015[7] K |
| Metallicity | 112% solar[13] |
| Rotation | 119 days[6] |
| Rotational velocity (v sin i) | 14[6] km/s |
| Age | 45 - 67?[14][15] Myr |
| α UMi Ab | |
| Mass | 1.316[9] M☉ |
| Radius | 1.04[3] R☉ |
| Luminosity (bolometric) | 3[3] L☉ |
| Age | >500?[15] Myr |
| α UMi B | |
| Mass | 1.39[3] M☉ |
| Radius | 1.38[7] R☉ |
| Luminosity (bolometric) | 3.9[7] L☉ |
| Surface gravity (log g) | 4.3[7] cgs |
| Temperature | 6900[7] K |
| Rotational velocity (v sin i) | 110[7] km/s |
| Age | 1.5?[14][15] Gyr |
| Other designations | |
| Polaris, North Star, Cynosura, Alpha UMi, α UMi, ADS 1477, CCDM J02319+8915 | |
| α UMi A: 1 Ursae Minoris, BD+88°8, FK5 907, GC 2243, HD 8890, HIP 11767, HR 424, SAO 308 | |
| α UMi B: NSV 631, BD+88°7, GC 2226, SAO 305 | |
| Database references | |
| SIMBAD | α UMi A |
| α UMi B | |
Polaris is a star in the northern circumpolar constellation of Ursa Minor. It is designated α Ursae Minoris (Latinized to Alpha Ursae Minoris) and is commonly called the North Star. With an apparent magnitude that fluctuates around 1.98,[3] it is the brightest star in the constellation and is readily visible to the naked eye at night.[16] The position of the star lies less than 1° away from the north celestial pole, making it the current northern pole star. The stable position of the star in the Northern Sky makes it useful for navigation.[17]
Although appearing to the naked eye as a single point of light, Polaris is a triple star system, composed of the primary, a yellow supergiant designated Polaris Aa, in orbit with a smaller companion, Polaris Ab; the pair is almost certainly[14] in a wider orbit with Polaris B. The outer companion B was discovered in August 1779 by William Herschel, with the inner Aa/Ab pair only confirmed in the early 20th century.
As the closest Cepheid variable, Polaris Aa's distance is a foundational part of the cosmic distance ladder. The revised Hipparcos stellar parallax gives a distance to Polaris A of about 432 light-years (ly) (133 parsecs (pc)), while the successor mission Gaia gives a distance of 446.5 ly (136.9 pc) for Polaris B[9][a].
Polaris Aa is an evolved yellow supergiant of spectral type F7Ib with 5.4 solar masses (M☉). It is the first classical Cepheid to have a mass determined from its orbit. The two smaller companions are Polaris B, a 1.39 M☉ F3 main-sequence star orbiting at a distance of 2,400 astronomical units (AU),[18] and Polaris Ab (or P), a very close F6 main-sequence star with a mass of 1.26 M☉.[3] In January 2006, NASA released images, from the Hubble telescope, that showed the three members of the Polaris ternary system.[19][20]
Polaris B can be resolved with a modest telescope. William Herschel discovered the star in August 1779 using a reflecting telescope of his own, one of the best telescopes of the time.[21]
The variable radial velocity of Polaris A was reported by W. W. Campbell in 1899, which suggested this star is a binary system.[22] Since Polaris A is a known cepheid variable, J. H. Moore in 1927 demonstrated that the changes in velocity along the line of sight were due to a combination of the four-day pulsation period combined with a much longer orbital period and a large eccentricity of around 0.6.[23] Moore published preliminary orbital elements of the system in 1929, giving an orbital period of about 29.7 years with an eccentricity of 0.63. This period was confirmed by proper motion studies performed by B. P. Gerasimovič in 1939.[24]
As part of her doctoral thesis, in 1955 E. Roemer used radial velocity data to derive an orbital period of 30.46 y for the Polaris A system, with an eccentricity of 0.64.[25] K. W. Kamper in 1996 produced refined elements with a period of 29.59±0.02 years and an eccentricity of 0.608±0.005.[26] In 2019, a study by R. I. Anderson gave a period of 29.32±0.11 years with an eccentricity of 0.620±0.008.[10]
There were once thought to be two more widely separated components—Polaris C and Polaris D—but these have been shown not to be physically associated with the Polaris system.[18][27]
Polaris Aa, the supergiant primary component, is a low-amplitude population I classical Cepheid variable, although it was once thought to be a type II Cepheid due to its high galactic latitude. Cepheids constitute an important standard candle for determining distance, so Polaris, as the closest such star,[10] is heavily studied. The variability of Polaris had been suspected since 1852; this variation was confirmed by Ejnar Hertzsprung in 1911.[29]
The range of brightness of Polaris is given as 1.86–2.13,[4] but the amplitude has changed since discovery. Prior to 1963, the amplitude was over 0.1 magnitude and was very gradually decreasing. After 1966, it very rapidly decreased until it was less than 0.05 magnitude; since then, it has erratically varied near that range. It has been reported that the amplitude is now increasing again, a reversal not seen in any other Cepheid.[6]
The period, roughly 4 days, has also changed over time. It has steadily increased by around 4.5 seconds per year except for a hiatus in 1963–1965. This was originally thought to be due to secular redward evolution across the Cepheid instability strip, but it may be due to interference between the primary and the first-overtone pulsation modes.[20][30][31] Authors disagree on whether Polaris is a fundamental or first-overtone pulsator and on whether it is crossing the instability strip for the first time or not.[11][31][32]
The temperature of Polaris varies by only a small amount during its pulsations, but the amplitude of this variation is variable and unpredictable. The erratic changes of temperature and the amplitude of temperature changes during each cycle, from less than 50 K to at least 170 K, may be related to the orbit with Polaris Ab.[12]
Research reported in Science suggests that Polaris is 2.5 times brighter today than when Ptolemy observed it, changing from third to second magnitude.[33] Astronomer Edward Guinan considers this to be a remarkable change and is on record as saying that "if they are real, these changes are 100 times larger than [those] predicted by current theories of stellar evolution".
Torres 2023 published a broad historical compilation of radial velocity and photometric data. He concludes that the change in the Cepheid period has reversed and is now decreasing since roughly 2010. Torres notes that TESS data is of limited utility: as a survey telescope, TESS is optimized for dimmer stars than Polaris, so Polaris significantly over-saturates TESS's cameras. Determining an accurate total brightness for Polaris from TESS is extremely difficult, although it remains suitable for timing the period.[34]
Furthermore, apparent irregularities in Polaris Aa's behavior may coincide with the periastron passage of Ab, although imprecision in the data prevents a definitive conclusion.[34] At the Gaia distance, the Aa-Ab closest approach is 6.2 AU; the radius of the primary supergiant is 46 R☉, meaning that the periastron separation is about 29 times its radius. This implies tidal forcing upon Aa's upper atmosphere by Ab. Such binary tidal forcing is known from heartbeat stars, where eccentric periastron approaches cause rich multimode pulsation akin to an electrocardiogram.
Szabados 1992 suggests that, among Cepheids, "phase slips" similar to what happened to Polaris in the mid 1960s are associated with binary systems.[35]
In 2024, researchers led by Nancy Evans at the Harvard & Smithsonian published a study with fresh data on the inner binary using the interferometric CHARA Array. They improved the solution of the orbit: combining CHARA data with previous Hubble data, and in tandem with the Gaia distance of 446±1 light-years, they confirmed the Cepheid radius estimate of 46 R☉ and re-determined its mass at 5.13±0.28 M☉. The corresponding Polaris Ab mass is 1.316±0.028 M☉. Polaris remains overluminous compared to the best Cepheid evolution models, something also seen in V1334 Cygni. Polaris's rapid period change and pulsation amplitude variations are still peculiar compared to other Cepheids, but may be related to the first-overtone pulsations.[9]
Evans et al also tentatively succeeded in imaging features on the surface of Polaris Aa: large bright and dark patches appear in close-up images, changing over time. Follow up imaging campaigns are required to confirm this detection.[9] Polaris's age is difficult to model; current best estimates find the Cepheid to be much younger than the two main sequence components, seemingly enough to exclude a common origin, which would be quite unlikely for a triple star system.[14][15]
Torres 2023 and Evans et al 2024 both suggest that recent literature cautiously agree that Polaris is a first overtone pulsator.[34][9]
Because Polaris lies nearly in a direct line with the Earth's rotational axis above the North Pole, it stands almost motionless in the sky, and all the stars of the northern sky appear to rotate around it. It thus provides a nearly fixed point from which to draw measurements for celestial navigation and for astrometry. The elevation of the star above the horizon gives the approximate latitude of the observer.[16]
In 2018 Polaris was 0.66° (39.6 arcminutes) away from the pole of rotation (1.4 times the Moon disc) and so revolves around the pole in a small circle 1.3° in diameter. It will be closest to the pole (about 0.45 degree, or 27 arcminutes) soon after the year 2100.[37] Because it is so close to the celestial north pole, its right ascension is changing rapidly due to the precession of Earth's axis, going from 2.5h in AD 2000 to 6h in AD 2100. Twice in each sidereal day Polaris's azimuth is true north; the rest of the time it is displaced eastward or westward, and the bearing must be corrected using tables or a rule of thumb. The best approximation[36] is made using the leading edge of the "Big Dipper" asterism in the constellation Ursa Major. The leading edge (defined by the stars Dubhe and Merak) is referenced to a clock face, and the true azimuth of Polaris worked out for different latitudes.
The apparent motion of Polaris towards and, in the future, away from the celestial pole, is due to the precession of the equinoxes.[38] The celestial pole will move away from α UMi after the 21st century, passing close by Gamma Cephei by about the 41st century, moving towards Deneb by about the 91st century.[citation needed]
The celestial pole was close to Thuban around 2750 BCE,[38] and during classical antiquity it was slightly closer to Kochab (β UMi) than to Polaris, although still about 10° from either star.[39] It was about the same angular distance from β UMi as to α UMi by the end of late antiquity. The Greek navigator Pytheas in ca. 320 BC described the celestial pole as devoid of stars. However, as one of the brighter stars close to the celestial pole, Polaris was used for navigation at least from late antiquity, and described as ἀεί φανής (aei phanēs) "always visible" by Stobaeus (5th century), also termed Λύχνος (Lychnos) akin to a burner or lamp and would reasonably be described as stella polaris from about the High Middle Ages and onwards, both in Greek and Latin. On his first trans-Atlantic voyage in 1492, Christopher Columbus had to correct for the "circle described by the pole star about the pole".[40] In Shakespeare's play Julius Caesar, written around 1599, Caesar describes himself as being "as constant as the northern star", although in Caesar's time there was no constant northern star. Despite its relative brightness, it is not, as is popularly believed, the brightest star in the sky.[41]
Polaris was referenced in the classic Nathaniel Bowditch maritime navigation book American Practical Navigator (1802), where it is listed as one of the navigational stars.[42]
The modern name Polaris[43] is shortened from the Neo-Latin stella polaris ("polar star"), coined in the Renaissance when the star had approached the celestial pole to within a few degrees.[44][45]
Gemma Frisius, writing in 1547, referred to it as stella illa quae polaris dicitur ("that star which is called 'polar'"), placing it 3° 8' from the celestial pole.[44][45]
In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[46] to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016 included a table of the first two batches of names approved by the WGSN; which included Polaris for the star α Ursae Minoris Aa.[47]
In antiquity, Polaris was not yet the closest naked-eye star to the celestial pole, and the entire constellation of Ursa Minor was used for navigation rather than any single star. Polaris moved close enough to the pole to be the closest naked-eye star, even though still at a distance of several degrees, in the early medieval period, and numerous names referring to this characteristic as polar star have been in use since the medieval period. In Old English, it was known as scip-steorra ("ship-star").[citation needed]
In the "Old English rune poem", the T-rune is apparently associated with "a circumpolar constellation", or the planet Mars.[48]
In the Hindu Puranas, it became personified under the name Dhruva ("immovable, fixed").[49]
In the later medieval period, it became associated with the Marian title of Stella Maris "Star of the Sea" (so in Bartholomaeus Anglicus, c. 1270s),[50] due to an earlier transcription error.[51]
An older English name, attested since the 14th century, is lodestar "guiding star", cognate with the Old Norse leiðarstjarna, Middle High German leitsterne.[52]
The ancient name of the constellation Ursa Minor, Cynosura (from the Greek κυνόσουρα "the dog's tail"),[53] became associated with the pole star in particular by the early modern period. An explicit identification of Mary as stella maris with the polar star (Stella Polaris), as well as the use of Cynosura as a name of the star, is evident in the title Cynosura seu Mariana Stella Polaris (i.e. "Cynosure, or the Marian Polar Star"), a collection of Marian poetry published by Nicolaus Lucensis (Niccolo Barsotti de Lucca) in 1655. [citation needed]
Its name in traditional pre-Islamic Arab astronomy was al-Judayy الجدي ("the kid", in the sense of a juvenile goat ["le Chevreau"] in Description des Etoiles fixes),[54] and that name was used in medieval Islamic astronomy as well.[55][56] In those times, it was not yet as close to the north celestial pole as it is now, and used to rotate around the pole.[citation needed]
It was invoked as a symbol of steadfastness in poetry, as "steadfast star" by Spenser. Shakespeare's sonnet 116 is an example of the symbolism of the north star as a guiding principle: "[Love] is the star to every wandering bark / Whose worth's unknown, although his height be taken."[57]
In Julius Caesar, Shakespeare has Caesar explain his refusal to grant a pardon: "I am as constant as the northern star/Of whose true-fixed and resting quality/There is no fellow in the firmament./The skies are painted with unnumbered sparks,/They are all fire and every one doth shine,/But there's but one in all doth hold his place;/So in the world" (III, i, 65–71). Of course, Polaris will not "constantly" remain as the north star due to precession, but this is only noticeable over centuries.[citation needed]
In Inuit astronomy, Polaris is known as Nuutuittuq (syllabics: ᓅᑐᐃᑦᑐᖅ).[58]
In traditional Lakota star knowledge, Polaris is named "Wičháȟpi Owáŋžila". This translates to "The Star that Sits Still". This name comes from a Lakota story in which he married Tȟapȟúŋ Šá Wíŋ, "Red Cheeked Woman". However, she fell from the heavens, and in his grief Wičháȟpi Owáŋžila stared down from "waŋkátu" (the above land) forever.[59]
The Plains Cree call the star in Nehiyawewin: acâhkos êkâ kâ-âhcît "the star that does not move" (syllabics: ᐊᒑᐦᑯᐢ ᐁᑳ ᑳ ᐋᐦᒌᐟ).[60]
In Mi'kmawi'simk the star is named Tatapn.[61]
In the ancient Finnish worldview, the North Star has also been called taivaannapa and naulatähti ("the nailstar") because it seems to be attached to the firmament or even to act as a fastener for the sky when other stars orbit it. Since the starry sky seemed to rotate around it, the firmament is thought of as a wheel, with the star as the pivot on its axis. The names derived from it were sky pin and world pin.[citation needed]
Since Leavitt's discovery of the Cepheid variable period-luminosity relationship, and corresponding utility as a standard candle, the distance to Polaris has been highly sought-after by astronomers. It is the closest Cepheid to Earth, and thus key to calibrating the Cepheid standard candle; Cepheids form the base of the cosmic distance ladder by which to probe the cosmological nature of the universe.[62]
Distance measurement techniques depend on whether or not components A and B are a physical pair, that is, gravitationally bound. If they are, then their estimated distance can be presumed to be equal.[b] Gravitational binding of this pair is well supported by observations, and the presumption of common distance is widely adopted in historical and recent estimates.[64][65][66][26][67][62][14][9]
For most of the 20th century, available observation technologies remained inadequate to precisely measure absolute parallax.[68][62] Instead, the main technique was to use theoretical models of stellar evolution for both main sequence and giant stars, combined with spectroscopic and photometric data to estimate distances. Such modeling relies on theoretical assumptions and guesses, and contains much systematic error and statistical uncertainties in population data. Even by 2013, these techniques were still struggling to achieve even 10% precision in either main sequence[69] or Cepheid[14] modeling.
Further progress was thus limited until the advent of Hipparcos, the first instrument able to engage in all-sky absolute parallax astrometry.[68] Its first data release was in 1997.
| Published | Component | Distance | Source | Notes | |
|---|---|---|---|---|---|
| ly | pc | ||||
| 1966 | B | (359)[c] | (110)[c] | Fernie[64] | Photometry and modeling of B[c] |
| 1977 | B | (399)[d] | (122)[d] | Turner[65] | Photometry and modeling of B[d] |
| 1978 | A | 356* | 109* | Gauthier and Fernie[66] | Modeling extinction and Cepheid evolution of A |
| 1996 | B | 359* | 110* | Kamper[26] | Photometry and modeling of B, reproducing prior estimates |
| 1997 | A | 431±29 | 132±9 | Hipparcos[70] | All-sky/absolute[68] parallax observations, of the primary variable[e] |
| 2004-2013 | A, B | 307±13 | 94±4 | Turner/Turner et al | Cepheid evolution modeling[30], cluster kinematics and ZAMS fitting[30][67], photometry and modeling of B[67], spectral line ratios of A calibrated on yellow supergiants[62] |
| 329±10 | 101±3 | ||||
| 323±7 | 99±2 | ||||
| 2007[f] | A | 432±6 | 133±2 | Hipparcos[2][69] | All-sky/absolute parallax observations, revised analysis, of the primary variable[f] |
| 2008 | B | 357* | 109.5* | Usenko & Klochkova[7] | Photometry and modeling of B |
| 2014 | A | >385 | >118 | Neilson[71] | Cepheid evolution modeling, independent of any distance prior |
| 2018 | B | 521±20 | 160±6 | Hubble, Bond et al.[14] | Relative[68] parallax of the wide component referencing photometrically-calibrated background stars |
| 2018 | B | 445.3±1.7 | 136.6±0.5 | Gaia DR2[72] | All-sky/absolute[68] parallax observations, of the wide component[g] |
| 2020 | B | 446.5±1.1 | 136.9±0.3 | Gaia DR3[5][9] | All-sky/absolute parallax observations, of the wide component[h] |
| ^ * This estimate didn't state its uncertainty |
After the arrival of the Hipparcos data, the distance to Polaris and consequent analysis of its Cepheid variation was controversial. The Hipparcos distance for Polaris was broadly but not universally adopted.[20] Immediately, the Hipparcos data for the nearest few hundred Cepheids appeared to clarify Cepheid models and to clear up then-tension in higher rungs of the distance ladder.[70] However alternatives remained; particularly by Turner et al, who published several papers between 2004 and 2013.[62]
In 2018, Bond et al[14] used the Hubble Space Telescope to provide an alternate direct measurement of Polaris's parallax; they summarize the back-and-forth:
However, Turner et al. (2013, hereafter TKUG13)[62] argue that the parallax of Polaris is considerably larger, 10.10 ± 0.20 mas (d = 99±2 pc). The evidence cited by TKUG13 for this “short” distance includes (1) a photometric parallax for Polaris B based on measured photometry, spectral classification, and main-sequence fitting; (2) a claim that there is a sparse cluster of A-, F-, and G-type stars within 3° of Polaris, with proper motions and radial velocities similar to that of the Cepheid, for which the Hipparcos parallaxes combined with main-sequence fitting give a distance of 99 pc; and (3) a determination of the absolute visual magnitude of Polaris based on line ratios in high-resolution spectra, calibrated against supergiants with well-established luminosities. [...]
[...]
In a critique of the TKUG13 paper, van Leeuwen (2013, hereafter L13)[69] defended the Hipparcos parallax by presenting details of the solution, concluding that “the Hipparcos data cannot in any way support” the large parallax advocated by TKUG13. Using Hipparcos data, L13 also questioned the reality of the sparse cluster proposed by TKUG13, presenting evidence against it both from the color versus absolute-magnitude diagram for stars within 3° of Polaris, and their non-clustered distribution of proper motions. Lastly, L13 examined the absolute magnitudes of nearly 400 stars of spectral type F3 V in the Hipparcos catalog with parallax errors of less than 10%, and showed that the absolute magnitude of Polaris B would fall well within the observed MV distribution for F3 V stars, based on either the Hipparcos parallax of A or the larger parallax proposed by TKUG13. Thus, he concluded that the photometric parallax of B does not give a useful discriminant.
— [14]
Bond et al go on to find a trigonometric parallax (independent of Hipparcos) that implies a distance further-still than the "long" Hipparcos distance, well outside the plausible range of the "short" distance estimates.
The next major step in high precision parallax measurements comes from Gaia, a space astrometry mission launched in 2013 and intended to measure stellar parallax to within 25 microarcseconds (μas).[74] Although it was originally planned to limit Gaia's observations to stars fainter than magnitude 5.7, tests carried out during the commissioning phase indicated that Gaia could autonomously identify stars as bright as magnitude 3. When Gaia entered regular scientific operations in July 2014, it was configured to routinely process stars in the magnitude range 3 – 20.[75] Beyond that limit, special procedures are used to download raw scanning data for the remaining 230 stars brighter than magnitude 3; methods to reduce and analyse these data are being developed; and it is expected that there will be "complete sky coverage at the bright end" with standard errors of "a few dozen μas".[76]
Gaia DR2 does not include a parallax for Polaris A, but a distance inferred from Polaris B is 136.6±0.5 pc (445.5±1.7 ly),[72] somewhat further than most previous estimates and (in principle) considerably more accurate. There are known to be considerable systematic uncertainties in DR2.[77]
Gaia DR3 significantly improved both the statistical and systematic uncertainties, although the latter remain numerous and on the order of 10–60 μas[63]; the new estimate is 136.9±0.3 pc (446.5±1.1 ly) using the baseline parallax zeropoint correction.[5][9][h]
Gaia DR4 (expected December 2026) will further improve the statistical and systematic uncertainties in general, and the data pipelines for variable and multiple stars in particular.[78] Multistar orbital solutions will become available, greatly aiding the study of Cepheids and Polaris, and in particular, may enable solving the outer AB orbit.[9]
Polaris is depicted in the flag and coat of arms of the Canadian Inuit territory of Nunavut,[79] the flag of the U.S. states of Alaska and Minnesota,[80] and the flag of the U.S. city of Duluth, Minnesota.[81][82]
Around 4800 years ago Thuban ( α Draconis) lay a mere 0°.1 from the pole. Deneb (
α Cygni) will be the brightest star near the pole in about 8000 years' time, at a distance of 7°.5.
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