Pleione (star)

28 Tauri is the star's Flamsteed designation and BU Tauri its variable star designation. The name Pleione originates with Greek mythology; she is the mother of seven daughters known as the Pleiades. In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN){{cite web | url=https://www.iau.org/science/scientific_bodies/working_groups/280/ | title=IAU Working Group on Star Names (WGSN)|access-date=22 May 2016}} to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016{{cite web | url=http://www.pas.rochester.edu/~emamajek/WGSN/WGSN_bulletin1.pdf | title=Bulletin of the IAU Working Group on Star Names, No. 1 |access-date=28 July 2016}} included a table of the first two batches of names approved by the WGSN; which included Pleione for this star. It is now so entered in the IAU Catalog of Star Names.{{cite web | url=http://www.pas.rochester.edu/~emamajek/WGSN/IAU-CSN.txt | title=IAU Catalog of Star Names |access-date=28 July 2016}}

{{Location mark

| image = Taurus constellation map.svg | type = thumb | float = left

| mark = Red circle.svg | mark_width = 20 | x = 810 | y = 323

| alt = Chart of the constellation Taurus

| caption = The location of the Pleiades (circled) in the constellation Taurus.

}}

With an apparent magnitude of +5.05 in V, the star is rather difficult to make out with the naked eye, especially since its close neighbour Atlas is 3.7 times brighter and located less than 5 arcminutes away.The brightness ratio of Atlas versus Pleione is derived from the formula for apparent magnitude and is based on their respective visual magnitudes: Atlas ($\{m\_A\}$) at 3.62 and Pleione ($\{m\_P\}$) at 5.05. Therefore:

:$\backslash frac\{m\_A\}\{m\_P\}=2.512^\{(5.05-3.62)\}=3.73$ Beginning in October of each year, Pleione along with the rest of the cluster can be seen rising in the east in the early morning before dawn.{{cite web

|last1=Getsova

|first1=I.

|display-authors=etal

|date=2002

|title=All About The Pleiades

|url=http://www.eso.org/public/outreach/eduoff/cas/cas2002/cas-projects/bulgaria_pleiades_1/

|work=Catch a Star 2002

|publisher=European Southern Observatory

|access-date=2010-09-15

|archive-date=2020-10-27

|archive-url=https://web.archive.org/web/20201027033628/http://www.eso.org/public/outreach/eduoff/cas/cas2002/cas-projects/bulgaria_pleiades_1/

|url-status=dead

}} To see it after sunset, one will need to wait until December. By mid-February, the star is visible to virtually every inhabited region of the globe, with only those south of 66° unable to see it. Even in cities like Cape Town, South Africa, at the tip of the African continent, the star rises almost 32° above the horizon. Due to its declination of roughly +24°, Pleione is circumpolar in the northern hemisphere at latitudes greater than 66° North. Once late April arrives, the cluster can be spotted briefly in the deepening twilight of the western horizon, soon to disappear with the other setting stars.

{{cite web

|last=Bakich |first=M. E.

|date=22 April 2009

|title=See Mercury, the Moon, and the Pleiades together in the night sky

|work=Astronomy

|url=http://www.astronomy.com/asy/default.aspx?c=a&id=8172

|access-date=2010-09-14

|quote=Don't miss a stunning sight around 9 P.M. local daylight time April 26 when a crescent Moon joins Mercury and the Pleiades in the deepening twilight.

}}

Pleione is classified as a Gamma Cassiopeiae type variable star, with brightness fluctuations that range between a 4.8 and 5.5 visual magnitude. It has a spectral classification of B8Vne, a hot main sequence star with "nebulous" absorption lines due to its rapid rotation and emission lines from the surrounding circumstellar disks formed of material being ejected from the star.

There has been significant debate as to the star's actual distance from Earth. The debate revolves around the different methodologies to measure distance—parallax being the most central, but photometric and spectroscopic observations yielding valuable insights as well.

For an in-depth discussion of Pleiades parallax measurements, see section 6.3 of {{cite journal

|last=van Leeuwen |first=F.

|date=2009

|title=Parallaxes and proper motions for 20 open clusters as based on the new Hipparcos catalogue

|journal=Astronomy and Astrophysics

|volume=497 |issue=1 |pages=209–242

|arxiv=0902.1039

|bibcode=2009A&A...497..209V

|doi=10.1051/0004-6361/200811382

|s2cid=16420237

}}

{{cite web

|last1=Allen |first1=J.

|last2=Boyd |first2=P.

|date=15 April 1997

|title=Finding Stellar Distances

|url=http://imagine.gsfc.nasa.gov/docs/ask_astro/answers/970415c.html

|work=Ask an Astrophysicist

|publisher=NASA

|access-date=2010-09-14

|quote=A straightforward summary of the different methods used by astronomers to measure stellar distances.

}} Before the Hipparcos mission, the estimated distance for the Pleiades star cluster was around 135 parsecs or 440 light years. When the Hipparcos Catalogue was published in 1997, the new parallax measurement indicated a much closer distance of about {{val|119|1.0|ul=pc}} ({{val|388|3.2|ul=ly}}), triggering substantial controversy among astronomers. The Hipparcos new reduction produced a broadly similar distance of {{val|120|2|u=pc}}. If the Hipparcos estimate were accurate, some astronomers contend, then stars in the cluster would have to be fainter than Sun-like stars—a notion that would challenge some of the fundamental precepts of stellar structure. Interferometric measurements taken in 2004 by the Hubble Telescope's Fine Guidance Sensors and corroborated by studies from Caltech and NASA's Jet Propulsion Laboratory showed the original estimate of 135 pc or 440 ly to be the correct figure. The Gaia EDR3 parallax is {{val|7.24|0.1255|ul=mas}}, indicating a distance around {{val|138|u=pc}}. This is relatively imprecise for a Gaia result due to the brightness of the star, but still with a statistical margin of error similar to the Hipparcos results.

In 1942 Otto Struve, one of the early researchers of Be Stars, stated that Pleione is "the most interesting member of the Pleiades cluster".

{{cite journal

|last=Struve |first=O.

|date=1943

|title=The Story of Pleione

|journal=Popular Astronomy

|volume=51 |page=233

|bibcode=1943PA.....51..233S

}} Like many of the stars in the cluster, Pleione is a blue-white B-type main sequence star with a temperature of about {{val|11,000|fmt=commas|ul=K}}. It has a bolometric luminosity of {{Solar luminosity|184|link=y}} assuming a distance of roughly 130 pc. With a radius of {{Solar radius|3.7|link=y}} and mass that is {{Solar mass|2.9|link=y}}, Pleione is considerably smaller than the brightest stars in the Pleiades. Alcyone for instance has a radius that is {{Solar radius|10|link=y}} with a luminosity {{Solar luminosity|2,400|link=y}}, making it roughly 30 times more voluminous than Pleione and about 13 times brighter.The relative size of Alcyone (V_A) compared to Pleione (V_P) is determined by comparing their volumes. It is assumed that the volume of each star is reasonably approximated by the formula for a sphere:

:V_A ≈ {{frac|4|3}}π × 10³ ≈ 4,188.79 V_Sun

:V_P ≈ {{frac|4|3}}π × 3.2³ ≈ 137.26 V_Sun

Therefore, the volume of Alcyone compared to Pleione ≈ 4,188.79 ÷ 137.26 ≈ 30.52

Alcyone's luminosity compared to Pleione is:

:2,400{{Solar luminosity|link=y}} ÷ 190{{Solar luminosity|link=y}} = 12.63 (or 13 rounded)

File:Classical Be star.jpg system. Classical Be stars like Pleione and Phi Persei exhibit gaseous equatorial disks, likely caused by rapid rotation.

{{cite web

|title=Classical Be Stars

|url=http://www.lehigh.edu/~mvm207/research.html

|work=Research in Astronomy & Astrophysics at Lehigh

|publisher=Lehigh University

|access-date=2010-09-16

}}]]

Pleione is a classical Be star, often referred to as an "active hot star".

{{cite web

|last=Stee |first=P.

|title=What is a Be star?

|work=Hot and Active Stars Research

|url=http://www.oca.eu/stee/page1/page3/page3.html

|access-date=2010-06-20

}} Classical Be stars are B-type stars close to the main sequence with the "e" in the spectral type signifying that Pleione exhibits emission lines in its spectrum, rather than the absorption lines typical of B-type stars.{{cite web

|last=Plait

|first=P.

|date=5 August 2009

|url=http://blogs.discovermagazine.com/badastronomy/2009/08/05/to-be-or-not-to-be/

|title=To B[e] or not to B[e]

|work=Bad Astronomy

|access-date=2010-09-20

|archive-date=2010-07-11

|archive-url=https://web.archive.org/web/20100711084034/http://blogs.discovermagazine.com/badastronomy/2009/08/05/to-be-or-not-to-be/

|url-status=dead

}} Emission lines usually indicate that a star is surrounded by gas. In the case of a Be star, the gas is typically in the form of an equatorial disk, resulting in electromagnetic radiation that emanates not just from the photosphere, but from the disk as well. The geometry and kinematics of this gaseous circumstellar environment are best explained by a Keplerian disk – one that is supported against gravity by rotation, rather than gas or radiation pressure.

{{cite journal

|last1=Porter |first1=J. M.

|last2=Rivinius |first2=T.

|date=2003

|title=Classical Be Stars

|journal=Publications of the Astronomical Society of the Pacific

|volume=115 |issue=812 |pages=1153–1170

|bibcode=2003PASP..115.1153P

|doi=10.1086/378307

|doi-access=free

}} Circumstellar disks like this are sometimes referred to as "decretion disks", because they consist of material being thrown off the star (as opposed to accretion disks which comprise material falling toward the star).{{cite web

|last = Thizy

|first = O.

|title = Be Stars

|url = http://www.shelyak.com/en/be_stars.html

|publisher = Shelyak Instruments

|access-date = 2010-06-20

|archive-url = https://web.archive.org/web/20110927005933/http://shelyak.com/dossier.php?id_dossier=24

|archive-date = 2011-09-27

|url-status = dead

}}

Be Stars are fast rotators (>200 km/s), causing them to be highly oblate, with a substantial stellar wind and high mass loss rate. Pleione's rotational velocity of {{val|329|u=km/s}} is considerably faster than the {{val|251|u=km/s}} of Achernar, a prototypical Be star. Pleione revolves on its axis once every 11.8 hours, compared to 48.4 hours for Achernar.The time it takes for Achernar (T_A) and Pleione (T_P) to rotate on its own axis is determined by taking the star's radius in solar units, multiplying by the Sun's radius in kilometers, then calculating the star's circumference at the equator and dividing by its speed of rotation per hour. Therefore:

:T_A = 10 {{Solar radius}} × 696,000 km × 2 × π ÷ 251 km/s ÷ 3,600 ≈ 48.4 hrs

:T_P = 3.2 {{Solar radius}} × 696,000 km × 2 × π ÷ 329 km/s ÷ 3,600 ≈ 11.8 hrs For comparison, the Sun takes 25.3 days to rotate. Pleione is spinning so fast that it is close to the estimated breakup velocity for a B8V star of about 370–390 km/s, which is why it is losing so much mass.

File:Alpha Arae.jpg rotating with a velocity close to breakup and losing mass through a stellar wind emerging from the poles.

{{cite press release

|display-authors=etal

|last1=Getsova |first1=I.

|title=To Be or Not to Be: Is It All About Spinning?

|date=20 September 2006

|publisher=European Southern Observatory

|url=http://www.eso.org/public/news/eso0635/

|access-date=2010-09-16

}}]]

Pleione is unusual because it alternates between three different phases: 1) normal B star, 2) Be star and 3) Be shell star. The cause is changes in the decretion disc, which appears, disappears, and reforms. Material in the disc is pulled back towards the star by gravity, but if it has enough energy it can escape into space, contributing to the stellar wind.{{cite web

|date=1 November 2002

|title=Glasgow astronomers explain hot star disks

|publisher=SpaceRef

|url=http://www.spaceref.com/news/viewpr.html?pid=9717

|archive-url=https://archive.today/20130202200315/http://www.spaceref.com/news/viewpr.html?pid=9717

|url-status=dead

|archive-date=February 2, 2013

|access-date=2010-06-20

}} Sometimes, Be stars form multiple decretion discs simultaneously, producing complex circumstellar dynamics.

File:BUTauLightCurve.png for Pleione]]

As a result of such dynamics, Pleione exhibits prominent long-term photometric and spectroscopic variations encompassing a period of about 35 years.

{{cite journal

|last1=Tanaka |first1=K.

|display-authors=etal

|date=2007

|title=Dramatic Spectral and Photometric Changes of Pleione (28 Tau) between 2005 November and 2007 April

|journal=Publications of the Astronomical Society of Japan

|volume=59 |issue=4 |pages=L35–L39

|url=http://pasj.asj.or.jp/v59/n4/590404/590404.pdf

|access-date=2010-06-13

|doi=10.1093/pasj/59.4.l35

|bibcode=2007PASJ...59L..35T

|doi-access=free

}} During the 20th century, Pleione went through several phase changes: it was in a Be phase until 1903, a B phase (1905–1936), a B-shell phase (1938–1954), followed by another Be phase (1955–1972).

{{cite journal

|last=Hirata |first=Ryuko

|date=1995

|title=Interpretation of the Long-Term Variation in Late-Type Active Be Stars

|journal=Publications of the Astronomical Society of Japan

|volume=47 |pages=195–218

|bibcode=1995PASJ...47..195H

}} It then returned to the Be-shell phase in 1972, developing numerous shell absorption lines in its spectrum. At the same time, the star showed a decrease in brightness, beginning at the end of 1971. After reaching a minimum brightness in late 1973, the star gradually re-brightened. In 1989, Pleione entered a Be phase which lasted until the summer of 2005.

These phase changes are ascribed to the evolution of a decretion disc that formed in 1972. Polarimetric observations show the intrinsic polarization angle has changed, indicating a change in orientation of the disc axis.

{{cite journal

|last=Hirata |first=R.

|date=2007

|title=Disk Precession in Pleione

|journal=ASP Conference Series

|volume=361 |page=267

|bibcode=2007ASPC..361..267H

}} Because Pleione has a stellar companion with a close orbit, the shift in the polarization angle has been attributed to the companion causing a precession (wobble) of the disk, with a precession period of roughly 81 years.

Photometric and spectroscopic observations from 2005 to 2007 indicated that a new disc had formed around the equator – producing a two discs at different inclination angles (60° and 30°). Such a misaligned double-disc structure had not been observed around other Be stars.

Pleione is known to be a speckle binary, although its orbital parameters have yet to be fully established.

{{cite journal

|last1=McAlister |first1=H. A.

|display-authors=etal

|date=1989

|title=ICCD speckle observations of binary stars. IV – Measurements during 1986–1988 from the Kitt Peak 4 M telescope

|journal=Astronomical Journal

|volume=97 |pages=510–531

|bibcode=1989AJ.....97..510M

|doi=10.1086/115001

}} In 1996 a group of Japanese and French astronomers discovered that Pleione is a single-lined spectroscopic binary with an orbital period of 218.0 days and a large eccentricity of 0.6.

{{cite journal

|author1=Katahira, Jun-Ichi

|display-authors=etal

|date=1996

|title=Period Analysis of the Radial Velocity in PLEIONE

|journal=Publications of the Astronomical Society of Japan

|volume=48 |issue=2

|pages=317–334

|bibcode=1996PASJ...48..317K

|doi=10.1093/pasj/48.2.317

|doi-access=free

}} The Washington Double Star Catalogue lists an angular separation between the two components of 0.2 arcseconds—an angle which equates to a distance of about 24 AU, assuming a distance of 120 parsecs.

{{cite web

|last1=Mason |first1=B. D.

|display-authors=etal

|date=1996

|title=Pleione

|url=http://www.alcyone.de/SIT/mainstars/SIT000781.htm

|publisher=Alcyone (Star Information Tool)

|access-date=2010-09-21

}}

File:Les Oceanides Les Naiades de la mer.jpg nymph. Painting from French artist Gustave Doré.]]

{{Main|Pleione (mythology)}}

Pleione was an Oceanid nymph of Mount Kyllene in Arkadia (southern Greece), one of the three thousand daughters of the Titans Oceanus and Tethys.

{{cite book

|last=Andrews |first=M.

|date=2004

|title=The Seven Sisters of the Pleiades – Stories from around the world

|url=https://books.google.com/books?id=3GbYg26S8pUC&pg=PA61

|publisher=Spinifex Press

|isbn=1-876756-45-4

|access-date=2010-10-07

}} The nymphs in Greek mythology were the spirits of nature; oceanids, spirits of the sea.

{{cite news

|last=Athena |first=A.

|date=8 July 2010

|title=Nymphs

|url=http://www.paleothea.com/Nymphs.html

|work=Women in Greek Myths

|access-date=2010-10-07

}} Though considered lesser divinities, they were still very much venerated as the protectors of the natural world. Each oceanid was thence a patroness of a particular body of water — be it ocean, river, lake, spring or even cloud — and by extension activities related thereto. The sea-nymph, Pleione, was the consort of Atlas, the Titan, and mother of the Hyas, Hyades and Pleiades.

When names were assigned to the stars in the Pleiades cluster, the bright pair of stars in the East of the cluster were named Atlas and Pleione, while the seven other bright stars were named after the mythological Pleiades (the 'Seven Sisters'). The term "Pleiades" was used by Valerius Flaccus to apply to the cluster as a whole, and Riccioli called the star Mater Pleione.

{{cite web

|last=Allen |first=R. H.

|date=1963

|title=Star Names: Their Lore and Meaning

|url=https://penelope.uchicago.edu/Thayer/E/Gazetteer/Topics/astronomy/_Texts/secondary/ALLSTA/Taurus*.html

|page=408

|publisher=Dover Publications

|access-date=2010-06-11

}}

There is some diversity of opinion as to the origin of the names Pleione and Pleiades. There are three possible derivations of note. Foremost is that both names come from the Greek word πλεῖν, (pr. ple'-ō), meaning "to sail".{{cite web

|last=Gibson

|first=S.

|date=5 April 2007

|title=Pleiades Mythology

|url=http://www.naic.edu/~gibson/pleiades/pleiades_myth.html

|publisher=National Astronomy and Ionosphere Center

|access-date=2010-06-18

|archive-date=2021-03-26

|archive-url=https://web.archive.org/web/20210326235401/http://www.naic.edu/~gibson/pleiades/pleiades_myth.html

|url-status=dead

}} This is particularly plausible given that ancient Greece was a seafaring culture and because of Pleione's mythical status as an Oceanid nymph. Pleione, as a result, is sometimes referred to as the "sailing queen" while her daughters the "sailing ones". Also, the appearance of these stars coincided with the sailing season in antiquity; sailors were well advised to set sail only when the Pleiades were visible at night, lest they meet with misfortune.

{{cite web

|author1=Apollodorus

|others=Translated by Frazer, J. G

|date=1921

|title=Book 3, Chapter 10, Section 1

|url=https://www.perseus.tufts.edu/hopper/text?doc=Apollod.%203.10.1&lang=original

|work=The Library

|access-date=2010-06-17

}}

Another derivation of the name is the Greek word Πλειόνη

{{cite web

|last=Smith |first=W.

|date=1873

|title=Plei'one

|work=A dictionary of Greek and Roman biography and mythology

|publisher=John Murray

|url=https://www.perseus.tufts.edu/hopper/text?doc=Perseus:text:1999.04.0104:entry=pleione-bio-1

|access-date=2010-06-17

}} (pr. plêionê), meaning "more", "plenty", or "full"—a lexeme with many English derivatives like pleiotropy, pleomorphism, pleonasm, pleonexia, plethora and Pliocene. This meaning also coincides with the biblical Kīmāh and the Arabic word for the Pleiades — Al Thurayya. In fact, Pleione may have been numbered amongst the Epimelides (nymphs of meadows and pastures) and presided over the multiplication of the animals, as her name means "to increase in number".

{{cite web

|last=Atsma |first=A. J.

|date=8 March 2010

|url=http://www.theoi.com/Nymphe/NymphePleione.html

|title=Pleione

|publisher=Theoi Greek Mythology

|access-date=2010-06-14

}}

Finally, the last comes from Peleiades ({{langx|grc|Πελειάδες|lit=doves}}), a reference to the sisters' mythical transformation by Zeus into a flock of doves following their pursuit by Orion, the [http://antwrp.gsfc.nasa.gov/apod/ap100329.html giant huntsman], across the heavens.

{{cite book

|author1=Hesiod

|author1-link=Hesiod

|others=Translated by Evelyn-White, H. G.

|date=1914

|chapter=ll. 618–640

|title=Works and Days

|url=http://www.sacred-texts.com/cla/hesiod/works.htm

|publisher=The Internet Sacred Text Archive

|access-date=2010-10-13

|isbn=0-585-30250-2

}}

In the best-selling 1955 nature book published by Time-Life called The World We Live In, there is an artist's impression of Pleione entitled Purple Pleione.

{{cite book

|last=Barnett |first=L.

|date=1955

|title=The World We Live In

|publisher=Simon & Schuster

|page=284

}} The illustration is from the famed space artist Chesley Bonestell and carries the caption: "Purple Pleione, a star of the familiar Pleiades cluster, rotates so rapidly that it has flattened into a flying saucer and hurled forth a dark red ring of hydrogen. Where the excited gas crosses Pleione's equator, it obscures her violet light."

Given its mythical connection with sailing and orchids, the name Pleione is often associated with grace, speed and elegance. Some of the finest designs in racing yachts have the name Pleione,

{{cite web

|title = Team Pleione

|publisher = Marblehead International One Design Class

|url = http://ww.marbleheadiod.com/8mr/

|access-date = 2010-10-07

}}{{dead link|date=January 2018 |bot=InternetArchiveBot |fix-attempted=yes }}

{{cite web

|last = Taylor

|first = J.

|date = 19 March 2009

|title = Fast Boats in the 'Spirit of Tradition'

|url = http://www.tayloryachtdesigns.com/yacht_design.php#post-33

|work = Jim Taylor Yacht Designs

|access-date = 2010-10-07

|url-status = dead

|archive-url = https://web.archive.org/web/20100217064337/http://www.tayloryachtdesigns.com/yacht_design.php#post-33

|archive-date = 17 February 2010

}} and the recent Shanghai Oriental Art Center draws its inspiration from an orchid.{{cite web

|last=Chami

|first=C.

|date=9 January 2008

|title=Paul Andreu – The Oriental Arts Centre in Shanghai

|url=http://www.archinnovations.com/featured-projects/public-buildings/paul-andreu-the-oriental-arts-centre-in-shanghai/

|publisher=Archinnovations

|access-date=2010-10-07

|archive-date=2012-03-07

|archive-url=https://web.archive.org/web/20120307080647/http://www.archinnovations.com/featured-projects/public-buildings/paul-andreu-the-oriental-arts-centre-in-shanghai/

|url-status=usurped

}} Fat Jon in his new album Hundred Eight Stars has a prismatic track dedicated to 28 Tauri.

{{discogs release|id=998205|name=Hundred Eight Stars}}

• Lists of stars in the constellation Taurus
• Class B Stars
• Be stars
• Shell star
• Circumstellar disk

{{Reflist|group=note}}

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}}

{{Commons category|Pleione (star)}}

• Jim Kaler's Stars, University of Illinois: [http://stars.astro.illinois.edu/sow/pleione.html PLEIONE (28 Tauri)]
• Philippe Stee's in-depth information on: [http://www.oca.eu/stee/page1/page3/page3.html Hot and Active Stars Research]
• Olivier Thizy's in-depth information on: [https://web.archive.org/web/20110927005933/http://shelyak.com/dossier.php?id_dossier=24 Be Stars]
• High-resolution LRGB image based on 4 hrs total exposure: [http://www.perseus.gr/Astro-DSO-M45.htm M45 – Pleiades Open Cluster]
• APOD Pictures:

1. [http://antwrp.gsfc.nasa.gov/apod/ap100329.html Orion, the giant huntsman, in pursuit of the Pleiades]
2. [http://antwrp.gsfc.nasa.gov/apod/ap091205.html Himalayan Skyscape]
3. [http://antwrp.gsfc.nasa.gov/apod/ap090212.html Pleiades and the Milky Way]
4. [http://antwrp.gsfc.nasa.gov/apod/ap071122.html Pleiades and the Interstellar Medium]

{{Stars of Taurus}}

{{Authority control}}

{{Good article}}

{{DEFAULTSORT:Pleione (Star)}}

Category:Taurus (constellation)

Category:Pleiades

Category:B-type main-sequence stars

Category:Be stars

Category:Gamma Cassiopeiae variable stars

Category:Binary stars

Tauri, 028

Tauri, BU

023862

1180

017851

BD+23 0558

Pleione