Bambancin rana

Bambancin rana
Bayanai
Ƙaramin ɓangare na	solar variation (en)
Fuskar	Sun's magnetic field (en)
Has immediate cause (en)	Solar dynamo (en)
Mai ganowa ko mai ƙirƙira	Heinrich Schwabe (en)
Time of discovery or invention (en)	1843
Nada jerin	list of solar cycles (en)

Tsarin hasken Rana, wanda aka fi sani da Tsarin aikin magnetic na hasken rana (sunspot cycle), ko kuma sake zagayowar Schwabe, canji ne na shekaru 11 a cikin aikin Sun wanda aka auna dangane da bambance-bambance a cikin yawan wuraren hasken rana da aka lura a saman Sun. A cikin lokacin sake zagayowar hasken rana, matakan hasken rana da fitar da kayan hasken rana. Adadin da girman Sunspots, hasken rana na hasken rana، da madauki na corona duk suna nuna canjin daidaitawa daga lokacin mafi ƙarancin aiki zuwa lokacin mafi ƙanƙanta aiki zuwa lokacin aiki.

Filin magnetic na Rana yana juyawa a lokacin kowane zagaye na rana, tare da juyawa yana faruwa lokacin da zagaye na hasken rana ya kusa da matsakaicin. Bayan zagaye biyu na hasken rana, filin magnetic na Sun ya koma asalinsa, ya kammala abin da aka sani da zagaye na Hale.

An lura da wannan sake zagayowar tsawon ƙarni ta hanyar canje-canje a bayyanar Sun da kuma abubuwan da ke faruwa a duniya kamar aurora amma ba a gano shi a sarari ba har zuwa 1843. Ayyukan hasken rana, wanda ke motsawa ta hanyar sake zagayowar hasken rana da matakai na lokaci-lokaci, yana sarrafa yanayin sararin samaniya ta hanyar ƙirƙirar yanayin sararin sama da tasirin sararin samaniya da ƙasa da kuma yanayin duniya da kuma yiwuwar sauye-sauyen yanayi a kan sikelin ƙarni da yawa.

Fahimtar da hasashen sake zagayowar hasken rana ya kasance daya daga cikin manyan ƙalubale a cikin astrophysics tare da manyan ramifications ga kimiyyar sararin samaniya da fahimtar abubuwan magnetohydrodynamic a wasu wurare a sararin samaniya.

Yarjejeniyar kimiyya ta yanzu game da canjin yanayi ita ce bambancin hasken rana kawai yana taka muhimmiyar rawa wajen fitar da canjin sauyin yanayi na duniya, tunda girman da aka auna na bambancin haskakawa na baya-bayan nan ya fi karami fiye da tilasta saboda iskar gas.

Samuel Heinrich Schwabe (1789-1875), masanin tauraron dan adam na Jamus, ya gano sake zagayowar rana ta hanyar fadada lura da sunspots.

Rudolf Wolf (1816-1893), masanin taurari na Switzerland, ya gudanar da sake gina tarihi na aikin hasken rana zuwa karni na 17.

Juyin halitta na magnetism a Rana

Ma'anar

Tsarin hasken rana yana da matsakaicin tsawon kimanin shekaru 11. Matsakaicin hasken rana da mafi ƙarancin hasken rana suna nufin lokutan matsakaicin ƙididdigar hasken rana. Hanyoyin zagaye sun kai daga mafi ƙanƙanta zuwa na gaba.

Tarihin lura

Tunanin sake zagayowar hasken rana na farko ya samo asali ne daga Christian Horrebow bisa ga abubuwan da ya lura na yau da kullun game da Sunspots da aka yi tsakanin 1761 da 1776 daga Rundetaarn observatory a Copenhagen, Denmark. A cikin shekara ta 1775, Horrebow ya lura da yadda "ya bayyana cewa bayan wasu shekaru, bayyanar Sun tana maimaita kanta dangane da yawan da girman tabo". Duk da haka ba za a gano zagaye na rana a sarari ba har zuwa 1843 lokacin da Samuel Heinrich Schwabe ya lura da bambancin lokaci-lokaci a cikin matsakaicin adadin sunspots bayan shekaru 17 na lura da hasken rana. Schwabe ya ci gaba da lura da sake zagayowar sunspot na wasu shekaru 23, har zuwa 1867. A cikin 1852, Rudolf Wolf ya sanya lambar farko ta hasken rana da ta fara a watan Fabrairun 1755 bisa ga Schwabe da sauran abubuwan lura. Wolf kuma ya kirkiro daidaitattun lambobin sunspot, Lambar Wolf, wanda ke ci gaba da amfani da ita a yau.

Tsakanin 1645 da 1715, an lura da ƙananan sunspots kuma an rubuta su. Gustav Spörer ne ya fara lura da wannan kuma daga baya aka kira shi Mafi ƙarancin Maunder bayan ƙungiyar matar-da-mijin Annie S. D. Maunder da Edward Walter Maunder waɗanda suka yi bincike sosai game da wannan lokaci na musamman.

A rabi na biyu na karni na sha tara Richard Carrington da Spörer da kansu sun lura da abubuwan da suka faru na sunspots da ke bayyana a wurare daban-daban na heliographic a sassa daban-daban nke sake zagayowar. (Dubi Dokar Spörer.) Alfred Harrison Joy daga baya zai bayyana yadda girman da aka "karkatar" sunspots - tare da babban wuri (s) kusa da ma'auni fiye da wuri (s). ― yana girma tare da latitude na waɗannan yankuna. (Dubi dokar Joy.)

George Ellery Hale da abokan aiki sun bayyana tushen sake zagayowar, wadanda a cikin 1908 suka nuna cewa sunspots suna da karfi sosai (bincike na farko na filayen magnetic bayan Duniya). A cikin 1919 sun gano alamu da yawa waɗanda za su zama sanannun Dokar Hale:

• A cikin wannan hemisphere na heliographic, yankuna masu aiki na bipolar suna da irin wannan polarity.
• A gefen da ke gaba (watau, a wancan gefen hasken rana) waɗannan yankuna suna da akasin haka.
• Jagoran polarities a cikin sassan biyu suna juyawa daga wani zagaye na sunspot zuwa na gaba.

Binciken Hale ya nuna cewa cikakken zagaye na magnetic - wanda daga baya za a kira shi da zagaye na Hale - ya ɗauki zagaye biyu na hasken rana, ko shekaru 22, kafin ya koma asalinsa (gami da polarity). Saboda kusan dukkanin bayyanar ba su da damuwa ga polarity, sake zagayowar hasken rana na shekaru 11 ya kasance mai mayar da hankali ga bincike; duk da haka, rabi biyu na sake zagayolar Hale yawanci ba iri ɗaya ba ne: sake zagayowan shekaru 11 yawanci suna canzawa tsakanin mafi girma da ƙananan adadin lambobin Wolf (Mulkin Gnevyshev-Ohl).

A cikin 1961 ƙungiyar uba da ɗa na Harold da Horace Babcock sun tabbatar da cewa zagaye na hasken rana tsari ne na sararin samaniya wanda ke bayyana a kan Rana gaba ɗaya. Sun lura cewa farfajiyar hasken rana tana da magnet a waje da sunspots, cewa wannan (mai rauni) filin magnetic shine farkon umarni na Dipole, kuma wannan dipole yana fuskantar juyawa na polarity tare da wannan lokacin kamar yadda zagaye na sunspot. Horace's Babcock Model ya bayyana filin magnetic na Sun kamar yadda yake da kusan daidaitattun shekaru 22. Ya rufe musayar makamashi tsakanin sassan tauraron rana da poloidal.