دنباله‌دار
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دنباله‌دار یک گلولهٔ برفی کیهانی است که از گازهای منجمد، سنگ و گرد و غبار ساخته‌شده و تقریباً به اندازهٔ یک شهر کوچک است.[۱] ساختار دنباله‌دار شامل سه بخش هسته، گیسو و دم است. هسته بخش مرکزی آن است و از گرد و غبار و گاز و یخ ساخته شده‌است. وقتی که دنباله‌دار نزدیک خورشید می‌شود، یخ‌های موجود در هستهٔ آن تبخیر می‌شود و تبدیل به ابر بزرگی پیرامون دنباله‌دار می‌شود که گیسو نام دارد. نیروی مغناطیسی بسیار قوی است و طناب‌ها، گره‌ها و نوارهایی تولید می‌کند که دم یونی را از دم گرد و غباری جدا می‌کند. سرچشمه و منشأ دنباله‌دارها، ابر اورت یا کمربند کویپر است. دنباله‌دارها، غیر دوره‌ای و دوره‌ای هستند که غیر دوره‌ای‌ها گرانش محدود به خورشید ندارند و مدار آن‌ها به شکل سهمی است. دنباله‌دارهای دوره‌ای نیز شامل دنباله‌دارهای بلند مدت (بسیار بیشتر از ۲۰۰ سال) و کوتاه مدت (۲۰ تا ۲۰۰ سال) است. در نام‌گذاری دنباله‌دارها، از نام کاشفان آن‌ها –یک شخص یا فضاپیما– استفاده می‌شود. اتحادیهٔ بین‌المللی اخترشناسی رهنمودی برای نام‌گذاری دنباله‌دارها مشخص کرده‌است. دنباله‌دارها تفاوت‌هایی با دیگر اجرام منظومهٔ خورشیدی از جمله سیارک‌ها، شهاب‌وارها، شهاب‌ها و شهاب‌سنگ‌ها دارند که مهم‌ترین آن‌ها چیزی است که آن‌ها از آن ساخته شده‌اند. برای نمونه، سیارک‌ها از فلزات و مواد سنگی و دنباله‌دارها از یخ، گرد و غبار و مواد سنگی ساخته شده‌اند. دنباله‌دارها انواع قابل‌توجهی مانند دنباله‌دار بزرگ و مسیر خورشیدی دارند. دنباله‌دارهای بزرگ آن‌قدر بزرگ نیستند که با چشم غیرمسلح دیده شوند؛ با این حال وقتی به خورشید نزدیک می‌شوند، سطوح یخی آن‌ها تبخیر می‌شود و مقدار زیادی از گاز و گرد و غبار آن‌ها فرار می‌کند و جو و دم‌های بسیار بزرگی شکل می‌گیرد که دیدنی و قابل‌توجه است. این دنباله‌دارها، دنباله‌دارهای بزرگ نامیده می‌شوند. دنباله‌دار مسیر خورشیدی نیز طبقهٔ ویژه‌ای از دنباله‌دارهاست که به هنگام حضیض خود، فاصلهٔ بسیار (حدود ۸۵۰٬۰۰۰ مایل) از خورشید دارند. در دوران باستان، دنباله‌دارها به عنوان پیامبران خدا در نظر گرفته می‌شدند. در فرهنگ‌های مختلف، آن‌ها عناوینی هم‌چون «پیشروی حکم مجازات» و «تهدید گیتی» به خود گرفته‌اند. برخی مانند کالین هامفریس، ستارهٔ بیت‌اللحم را یک دنباله‌دار می‌دانند که در انجیل متی ذکرشده و راهنمای سه مغ به زادگاه عیسی مسیح است. محتویاتپیشینهٔ مطالعه[ویرایش] متنی به زبان آلمانی دربارهٔ اثرات یک دنباله‌دار در سدهٔ هفدهم میلادی در زمان‌های گذشته، دنباله‌دارها به عنوان پیشگویان فاجعه‌ها و پیامبران خدا در نظر گرفته می‌شدند.[۲] در سال ۱۰۸۰–۱۰۷۰ میلادی، دنباله‌دار هالی در فرشینه بایو (که تاریخچهٔ نبرد هیستینگز را به تصویر می‌کشد) به تصویر کشیده‌شد. در سال ۱۴۵۰–۱۴۴۹، ستاره‌شناسان نخستین تلاش‌ها برای ثبت مسیر دنباله‌دارها در آسمان شب را انجام‌دادند. در سال ۱۷۰۵، ادموند هالی تشخیص داد که دنباله‌دارهایی که در سال ۱۵۳۱، ۱۶۰۷ و ۱۶۸۲ دیده شده‌است، در واقع یک دنباله‌دار است و پیش‌بینی کرد که دوباره در سال ۱۷۵۸ دیده خواهد شد. از آن پس این دنباله‌دار، دنباله‌دار هالی نام گرفت. در سال ۱۹۹۴، در نخستین مشاهدهٔ برخورد سیاره و دنباله‌دار، دانشمندان از تماشای برخورد دنبالهٔ دار شومیکر-لوی ۹ با جو مشتری شگفت‌زده شدند. در سال ۲۰۰۴، فضاپیمای استارداست نمونه‌های گرد و غبار از دنباله‌دار ویلد ۲ جمع‌آوری کرد. در سال ۲۰۰۵، فضاپیمای برخورد ژرف با دنباله‌دار تمپل ۱ برخورد کرد تا درون هستهٔ آن را آشکار کند.[۳] سرچشمه و منشأ[ویرایش]تئوری ریاضی نشان می‌دهد که ممکن‌است که بسیاری از دنباله‌دارها از مناطق بسیار دور (حدود ۱۰۰٬۰۰۰ واحد نجومی) در منظومهٔ خورشیدی سرچشمه بگیرند. هر یک واحد نجومی به اندازهٔ فاصلهٔ میان زمین و خورشید و حدود ۱۰۰٬۰۰۰٬۰۰۰ مایل است. فاصلهٔ سیارهٔ بهرام از خورشید ۱/۵، سیارهٔ برجیس از خورشید ۵ و پلوتو از خورشید ۳۹ واحد نجومی است؛ بنابراین، دنباله‌دارها از مناطق بسیار دور سرچشمه می‌گیرند. دنباله‌دارها از تمام جهات به سوی منظومهٔ خورشیدی می‌آیند؛ بنابراین جایی که آن‌ها از آن سرچشمه می‌گیرند، باید منطقه‌ای غول‌پیکر در پیرامون منظومهٔ خورشیدی باشند. اما برخی از آن‌ها از منطقه‌ای نزدیک‌تر به نام کمربند کویپر سرچشمه می‌گیرند.[۴]  پراکندگی اجسام کمربند کویپر (اجسام سبز رنگ) در منظومهٔ خورشیدی در سال ۱۹۴۳، ستاره‌شناسی به نام کنت اجورس گفت که مخزنی برای دنباله‌دارها و اجسام بزرگ‌تر، فراتر از سیارات وجود دارد. در سال ۱۹۵۰، ستاره‌شناسی هلندی به نام یان اورت گفت که دنباله‌دارها از جایی بسیار دور در پیرامون منظومهٔ خورشیدی می‌آیند. او نام این منطقه را ابر اورت گذاشت که اشیاء انبوهی در این ابر غول‌پیکر وجود دارند. ابر اورت فضایی به اندازهٔ ۱۰۰٬۰۰۰–۵٬۰۰۰ واحد نجومی را اشغال می‌کند و در منطقه‌ای از فضا قرار دارد که تأثیر گرانش خورشید بر آن ضعیف‌تر از تأثیر گرانش ستاره‌های مجاور بر آن است. ابر اورت احتمالاً دارای ۱۰۰ میلیارد تا ۲ تریلیون جسم یخی در مدار خورشیدی است.[۳] در سال ۱۹۵۱، ستاره‌شناسی به نام جرارد کویپر نظریه‌ای ارائه داد که یک کمربند دیسک مانند در حوزهٔ پلوتو وجود دارد که در آن اجرام یخی فرانپتونی و اجتماعی از دنباله‌دارها وجود دارد. گاهی اوقات این اجرام یخی توسط گرانش به مداری پیرامون خورشید هل داده می‌شوند و تبدیل به دنباله‌دارهای با تناوب مداری کوتاه می‌شوند.[۵] اگرچه شمار کمی از دنباله‌دارها از کمربند کویپر می‌آیند، اما بسیاری از آن‌ها از ابر اورت سرچشمه می‌گیرند. وقتی که ستارگان در حال گذر در فضا هستند، به برخی از اشیاء ابر اورت که خارج از مدارهای خود هستند، برخورد می‌کنند و دنباله‌دارها ساخته می‌شوند. بیشتر دنباله‌دارهای با تناوب مداری کوتاه از کمربند کویپر و با تناوب مداری بلند از ابر اورت سرچشمه می‌گیرند؛ هر چند که چند مورد استثنا برای این قاعده وجود دارد. برای نمونه، دنباله‌دار هالی تناوب مداری کوتاهی دارد و از ابر اورت سرچشمه گرفته‌است.[۶] بررسی اجمالی[ویرایش]ویژگی‌ها[ویرایش] دنباله‌دار هالی استثنایی است و بر خلاف این که دورهٔ مداری کوتاهی دارد، از ابر اورت سرچشمه گرفته‌است.[۶] دنباله‌دارها، غیر دوره‌ای و دوره‌ای هستند. دنباله‌دارهای غیر دوره‌ای که از ابر اورت می‌آیند، گرانش محدود به خورشید ندارند و مدار آن‌ها به شکل سهمی است و تنها یک بار خورشید را می‌بینند و هرگز دوباره باز نمی‌گردند.[۷] دنباله‌دارهای دوره‌ای نیز شامل دنباله‌دارهای بلند مدت (بسیار بیشتر از ۲۰۰ سال) و کوتاه مدت است که به ترتیب از ابر اورت و کمربند کویپر سرچشمه می‌گیرند.[۸] ویژگی‌ها و رفتار دنباله‌دارهایی که از ابر اورت ۰ تا ۲۰۰ سال) هستند و ویژگی‌های مداری آن‌ها نیز متفاوت است. دو خانوادهٔ بزرگ از دنباله‌دارهای کوتاه مدت وجود دارد: نخست خانوادهٔ برجیس با دورهٔ کمتر از ۲۰ سال و دوم خانوادهٔ هالی با دورهٔ ۲۰ تا ۲۰۰ سال.[۸] تفاوت‌های دینامیکی این دو گروه ناشی از تأثیر اجسام دیگر است. اجسام ابر اورت توسط رویدادهایی که فراتر از منظومهٔ خورشیدی رخ می‌دهد، آشفته می‌شوند. اما دنباله‌دارهای کمربند کویپر به‌طور مستقیم توسط هیچ ستاره‌ای به جز خورشید نمی‌توانند آشفته شوند. اگر خورشید از کنار ستارهٔ دیگری (یا یک ابر بزرگ مولکولی) بگذرد، دنباله‌دارها در مداری بیضی‌شکل و به سمت منظومهٔ خورشیدی به گردش در می‌آیند. اما سیارهٔ نپتون که بسیار نزدیک به کمربند کویپر است، نقش مهمی در ثبات مدار اجسام کمربند یا برعکس هل دادن اجسام به دورتر از مدار پیشین خود دارند.[۸] ترکیبات شیمیایی دنباله‌دارهای بلند مدت و کوتاه مدت مشابه است، اگرچه ترکیبات سازندهٔ دنباله‌دارهای بلند مدت تمایل بیشتری به فرار دارند. دلیل این تفاوت می‌تواند سرچشمه‌گیری از ابر اورت یا کمربند کویپر باشد. در واقع در طول شکل‌گیری منظومهٔ خورشیدی، اجسام کوچک در بخش‌های درونی دیسک و در نزدیکی سیارات غول‌پیکر ساخته‌شدند. سپس این اجسام توسط نیروهای گرانشی از منظومهٔ خورشیدی خارج شدند و آن اجسامی که به‌طور کامل فرار کردند، ابر اورت را تشکیل دادند. آن دسته از اجسامی که نتوانستند فرار کنند و هیچ تعامل گرانشی با سیارات نداشتند، به عنوان اجسام کمربند کویپر باقی‌ماندند.[۸] نام‌گذاری[ویرایش] نام‌گذاری دنباله‌دارها پیچیده است و نام آن‌ها از روی کاشفشان –یک شخص یا فضاپیما– برگرفته می‌شود. برای نمونه، دنباله‌دار شومیکر-لوی ۹ نهمین دنباله‌داری بود که توسط یوجین مرل و کارولین شومیکر و دیوید لوی کشف شده‌است. این رهنمود توسط اتحادیهٔ بین‌المللی اخترشناسی تنها در سدهٔ گذشته ایجاد شده‌است. از آن‌جا که فضاپیماها در نقطه بینی دنباله‌دارها بسیار مؤثر است، دنباله‌دارها در نام‌های خود نام فضاپیماهایی هم‌چون سوهو و وایز را دارند.[۳] اتحادیهٔ بین‌المللی اخترشناسی روشی را برای نام‌گذاری دنباله‌دارها برگزیده‌است. این نام‌گذاری چهار مرحله دارد: ۱. ابتدا باید یکی از پیشوندهای زیر را برای اشاره به نوع دنباله‌دارها مشخص کرد. این پیشوندها عبارتند از:
۲. سپس سال کشف دنباله‌دار را می‌نویسند. ۳. در این مرحله، حرف بزرگ A یا B را برای فهمیدن این که دنباله‌دار در نیمهٔ نخست ماه کشف شده‌است یا نیمهٔ دوم ماه، می‌نویسند. حرف بزرگ A را برای اشاره به نیمهٔ نخست ماه و حرف بزرگ B را برای اشاره به نیمهٔ دوم ماه می‌نویسند. ۴. در این مرحله، عددی می‌نویسند که نشان‌دهندهٔ چندمین جسمی است که در آن سال و آن نیمهٔ ماه کشف شده‌است. برای نمونه، P/۲۰۱۳ B۳ سومین دنباله‌دار کشف‌شده در نیمهٔ دوم ژانویهٔ ۲۰۱۳ است. وقتی که یک دنباله‌دار برای دومین بار آشکار و مشاهده می‌شود، مرکز ریزسیارهٔ اتحادیهٔ بین‌المللی اخترشناسی (MPC) یک شمارهٔ دائمی برای کشف آن می‌دهد. در این حالت، ابتدای نام دنباله‌دار، نام دو کاشف آن (نام خانوادگی فرد یا یک واژه یا مخفف گروه اخترشناسی) را می‌نویسند. نام‌ها به ترتیب زمانی پدیدار می‌شوند و نام کاشفان و ترتیب زمانی با یک ممیز از یک‌دیگر جدا می‌شوند. اما در برخی موارد نادر، نام دنباله‌دار می‌تواند شامل نام سه کاشف یا عمومی باشد. نمونه‌هایی از نام‌های کامل این دنباله‌دارها عبارتند از: ۱۱۹پی/پارکر–هارتلی و سی۱۹۹۵/اُ۱ (دنباله‌دار هیل–باپ).[۹] مأموریت‌ها[ویرایش]فهرست زیر، مأموریت‌هایی است که برای بررسی دنباله‌دارها انجام گرفته‌است:[۱۰][۱۱]
ساختار[ویرایش]هسته[ویرایش] قطر دنباله‌دار ۲۹پی/شواسمن-واچمن احتمالاً حدود ۲۰ کیلومتر است. (نگاره‌ای با رنگ‌های کاذب و دروغین از تلسکوپ فضایی اسپیتزر) هسته یا قلب دنباله‌دار تکه‌های جامدی در مرکز گیسوی آن و مانند یک گلولهٔ برفی ناپاک است که از یخ ساخته شده‌است.[۲۹] هسته که بخش مرکزی دنباله‌دار است، مخزن گرد و غبار و گازهای منجمد است.[۳۰] هستهٔ دنباله‌دار اسفنجی شکل است و درون آن شمار بسیار چاله و حفره وجود دارد. هنوز هیچ‌کسی نمی‌داند که هسته دارای حفره‌های کم و بزرگ یا حفره‌های بسیار و کوچک است. اگر شمار کمی حفرهٔ بزرگ بر روی هسته وجود داشته‌باشد، یعنی این که این دنباله‌دار از سنگ‌های یخی ناپاک ساخته‌شده و اگر شمار بسیاری حفرهٔ کوچک بر روی آن وجود داشته‌باشد، یعنی این که این دنباله‌دار از گلوله‌های یخی ناپاک ساخته شده‌است.[۲۹] هسته از نوع خاصی از گرد و غبار به نام «کرکی» ساخته شده‌است، چون کرکی می‌تواند سبک وزن و پر از سوراخ مانند اسفنج باشد. درون سوراخ‌ها از یخ آب مانند، کربن دی‌اکسید (یخ خشک) و کربن مونوکسید (که از خودروها خارج می‌شود) ساخته شده‌است.[۳۱] لایه‌های بالایی هسته از گرد و غبار ساخته شده‌است. گرد و غبار غیر فرار متشکل از برخی کانی‌های سیلیکات و غنی از کربن، هیدروژن، اکسیژن و نیتروژن است. در هسته، نسبت جرم فرار به جرم غیر فرار نزدیک به یک است.[۳۰] مشاهدات هستهٔ دنباله‌دارهای هیل-باپ و کوهوتک به دانشمندان ایده‌های تازه دربارهٔ ترکیب و تکامل دنباله‌دارها داده‌است. اما هنوز دانشمندان نمی‌دانند که آیا هستهٔ دنباله‌دارها مانند بخش‌های جامد زمین، سخت یا مانند یک گلولهٔ برفی، نرم است. کاوشگر فضایی رزتا برای یافتن میزان سختی دنباله‌دارها امیدوارکننده است. وقتی که دنباله‌دار به خورشید نزدیک می‌شود، شروع به تبخیر می‌کند و یک گیسو و یک دم دیدنی و جذاب پدید می‌آید. این تبخیر تنها در جاهای خاص هسته روی می‌دهد که «جت» نامیده می‌شود. دنباله‌دار هالی هنگامی که در سال ۱۹۸۶ به خورشید نزدیک می‌شد، بر روی سطح خود سه جت داشت.[۳۱] اندازهٔ هسته معمولاً ناشناخته است، زیرا اندازه‌گیری آن دشوار است، اما اندازه‌گیری قابل اطمینانی از ۱۰ هستهٔ دنباله‌دار به عمل آمده‌است. بسیاری از این هسته‌ها دارای قطرهای چند کیلومتر تا ۱۰ تا ۲۰ کیلومتر هستند. برای نمونه، هستهٔ ۲۹پی/شواسمن-واچمن احتمالاً حدود ۲۰ کیلومتر و قطر دنباله‌دار هیل-باپ احتمالاً ۴۰ کیلومتر است. البته موارد خاصی مانند دنباله‌دار هالی و ۱۹پی/بورلی دارای هسته‌ای سیب‌زمینی‌شکل هستند.[۳۰] گیسو[ویرایش] ابر پیرامون دنباله‌دار سی/۱۹۸۳ اچ۱، گیسوی آن است. وقتی که یخ‌های موجود در هستهٔ دنباله‌دار تبخیر می‌شود، تبدیل به یک ابر بزرگ پیرامون بخش مرکزی دنباله‌دار می‌شود و به سرعت گسترش می‌یابد. این ابر که گیسو نامیده می‌شود، جو دنباله‌دار است و می‌تواند تا میلیون‌ها مایل گسترش یابد. این ابر بسیار نازک و باریک و ۱۰٬۰۰۰ بار نازک‌تر و باریک‌تر از یک ابر در جو زمین است.[۳۲] هنگامی که دنباله‌دار در حضیض خود است، گیسوی آن معمولاً حدود ۱۰۰٬۰۰۰ کیلومتر و توسط باد خورشیدی مانند یک قطرهٔ اشک درآمده‌است.[۳۳] گیسوی دنباله‌دارها دارای دو جزء اصلی است: ۱. گیسوی گازی: متشکل از مولکول‌های آزادشده از هسته توسط گرمایش خورشیدی و تصعید است. هنگامی که هستهٔ دنباله‌دار آشکار است، مولکول‌های گیسوی آن در معرض تابش مستقیم خورشید قرار می‌گیرند و می‌توانند به شیوه‌های مختلف آسیب ببینند. سپس بیشتر مولکول‌ها از هم جدا و از هسته خارج می‌شوند. برای نمونه: H + HO → فشار قوی + H۲O H + O → فشار قوی + OH در واکنش‌های بالا، مولکول آزادشده از هسته یک فوتون جذب می‌کند و به دو قطعه شکسته می‌شود. علاوه بر این، گونه‌های گازی دنباله‌دارها می‌توانند یونیزه شوند. مانند واکنش زیر: CO+ → فشار قوی + CO ۲. گیسوی گرد و غباری: متشکل از ذرات گرد و غبار کشانده‌شده از هسته است. ذرات گرد و غبار دنباله‌دارها در همهٔ اندازه‌ها یافت می‌شوند و قابل رؤیت‌ترین آن‌ها قطری حدود ۱ میکرون (۰/۰۰۱ میلی‌متر) دارد.[۳۴] دم[ویرایش] دم دنباله‌دار سی/۲۰۰۶ پی۱ بسیار بلند و کشیده است.  دم یونی آبی رنگ دنباله‌دار ۱۷پی هولمز در سمت راست آن دیده می‌شود. به‌طور کلی، دنباله‌دارها دارای دو نوع دم هستند:[۳۵] ۱. دم یونی: گازهای خنثی در گیسوی دنباله‌دار می‌توانند توسط فوتون‌های فرابنفش خورشیدی یونیزه شوند. مانند واکنش زیر: CO+ → فشار قوی + CO میدان مغناطیسی ستاره‌ای خورشید توسط بادهای خورشیدی جابه‌جا می‌شود و هم‌چنین یون‌ها نیز به نیروهای مغناطیسی حساسند. در نتیجه، یون‌ها از گیسو پاک‌سازی می‌شوند و درون یک دم یونی بلند می‌روند. از آن‌جا که CO+ شایع‌ترین یون است، نور آبی بهتر از نور قرمز پراکنده می‌شود و دم یونی به چشم انسان اغلب آبی رنگ به نظر می‌رسد. هم‌چنین، نیروی مغناطیسی بسیار قوی است و طناب‌ها، گره‌ها و نوارهایی تولید می‌کند که دم یونی را از دم گرد و غباری جدا می‌کند. ۲. دم گرد و غباری: متشکل از ذرات گرد و غبار رانده‌شده از گیسو توسط فشار ناشی از تابش خورشیدی است. در مقایسه با دم یونی، دم گرد و غباری به نظر می‌رسد که سفید رنگ یا کمی صورتی رنگ باشد. ذرات گرد و غبار دم دنباله‌دارهایی که به صورت جداگانه در مداری پیرامون خورشید هستند، به دلیل اثر فشار تابشی، گرانش آن‌ها به خورشید کمتر از گرانش آن‌ها به هسته است. این موجب می‌شود که دم گرد و غباری خمیده و منحنی باشد.[۳۶] دنباله‌دارهای قابل‌توجه[ویرایش]دنباله‌دارهای بزرگ[ویرایش] شمار کمی از دنباله‌دارها که دیدنی و قابل‌توجه و چشمگیر هستند، با عنوان «دنباله‌دارهای بزرگ» شناخته می‌شوند؛ فقط باید مجموعه‌ای از شرایط رخ‌دهد. این دنباله‌دارها آن‌قدر بزرگ نیستند که با چشم غیرمسلح دیده شوند؛ با این حال وقتی به خورشید نزدیک می‌شوند، سطوح یخی آن‌ها تبخیر می‌شود و مقدار زیادی از گاز و گرد و غبار آن‌ها فرار می‌کند و جو و دم‌های بسیار بزرگی شکل می‌گیرد که دیدنی و قابل‌توجه است. اگر این شرایط رخ‌دهد، دنباله‌دار تبدیل به یک دنباله‌دار بزرگ خواهد شد. علاوه بر این، اگر دنباله‌دار نزدیک زمین شود و دم آن به آسانی دیده شود، عنوان دنباله‌دار بزرگ را به خود می‌گیرد. در هر دو مورد، دنباله‌دار بزرگ باید در آسمان تاریک دیده شود. در ژوئیهٔ سال ۸۷ پیش از میلاد، نخستین دنباله‌دار بزرگ که دنباله‌دار هالی بود، در آسمان دیده‌شد.[۳۷] دنباله‌دار مسیر خورشیدی[ویرایش]دنباله‌دار مسیر خورشیدی طبقهٔ ویژه‌ای از دنباله‌دارهاست که به هنگام حضیض خود، فاصلهٔ بسیار کمی (حدود ۸۵۰٬۰۰۰ مایل) با خورشید دارند. حتی بسیاری از آن‌ها به فاصلهٔ چند هزار مایلی خورشید نیز می‌رسند. ماندن در این فاصله از خورشید برای دنباله‌دارها بسیار دشوار است. آن‌ها در معرض تابش خورشیدی قرار می‌گیرند؛ البته فشار فیزیکی تابش خورشیدی به شکل‌گیری دم دنباله‌دارها کمک می‌کند. علاوه بر این، دنباله‌دارها در نزدیکی خورشید، نیروهای جزر و مد بسیار قوی یا فشار گرانشی را تجربه می‌کنند. در این محیط خصمانه و دشمن‌وار، بسیاری از دنباله‌دارها با این سفر پیرامون خورشید دیگر زنده نمی‌مانند و از میان می‌روند. اگرچه آن‌ها به سطح خورشید سقوط نمی‌کنند، اما خورشید می‌تواند آن‌ها را از میان ببرد. بسیاری از دنباله‌دارهای که دارای مدارهای مشابه هستند، «کروز پاس» نامیده می‌شوند و جمعی دیگر متعلق به گروهی به نام «گروه کروز» هستند. نزدیک به ۸۵ درصد دنباله‌دارها توسط دنباله‌دار سوهو در این بزرگراه مداری دیده می‌شوند. دانشمندان بر این باورند که صدها یا هزاران سال پیش، یک دنباله‌دار مسیر خورشیدی وجود داشت که فروپاشید و دنباله‌دارهای کروز پاس باقی‌ماندهٔ آن‌ها هستند. در ۲۸ نوامبر ۲۰۱۳، سی/۲۰۱۲ اس۱ به حضیض خود (۷۳۰٬۰۰۰ مایل فاصله از خورشید) خواهد رسید. مدار این دنباله‌دار نشان می‌دهد که می‌تواند با این حرکت از منظومهٔ خورشیدی فرار کند.[۳۸] موضوعات مرتبط[ویرایش]تفکیک از اجرام آسمانی دیگر[ویرایش] یک بارش شهابی اسدی در سال ۲۰۰۹ تفاوت اصلی میان دنباله‌دارها و سیارک‌ها چیزی است که آن‌ها از آن ساخته شده‌است. سیارک‌ها از فلزات و مواد سنگی و دنباله‌دارها از یخ، گرد و غبار و مواد سنگی ساخته شده‌اند. هر دو جسم آسمانی حدود ۴/۵ میلیارد سال پیش در اوایل منظومهٔ خورشیدی ساخته‌شدند. سیارک‌ها نسبت به دنباله‌دارها بسیار نزدیک‌تر به خورشید هستند، جایی که برای باقی ماندن یخ به حالت جامد بسیار گرم است. اما دنباله‌دارها نسبت به سیارک‌ها دورتر از خورشید هستند، جایی که یخ در آن ذوب نمی‌شود. یکی دیگر از تفاوت‌های میان این دو جسم آسمانی این است که دنباله‌دارها دم دارند و سیارک‌ها فاقد دم هستند. از دیگر تفاوت‌های این دو شیء فضایی می‌توان به الگوهای مداری آن‌ها اشاره کرد. دنباله‌دارها به مدارهای بسیار طولانی و دراز تمایل دارند و چندین بار ۵۰٬۰۰۰ واحد نجومی از خورشید فاصله می‌گیرند. در حالی که سیارک‌ها به مدارهای کوتاه‌تر و دایره‌ای‌شکل‌تر تمایل و در کمربند سیارک‌ها وجود دارند. تعداد دو شیء فضایی از تفاوت‌های دیگر آن‌هاست. تنها ۳٬۵۷۲ دنباله‌دار تا ۲۰ ژوئن ۲۰۰۹ کشف شده‌است، اما میلیون‌ها سیارک وجود دارد.[۳۹] بقایای کوچک‌تر از یک سیارک، شهاب‌وار نامیده می‌شود. بیشتر شهاب‌وارهایی که وارد جو زمین می‌شوند، به اندازه‌ای کوچک هستند که نمی‌توانند وارد سطح زمین شوند و تبخیر می‌شوند و در این حالت عناوین مختلفی (شهاب یا شهاب‌سنگ) می‌گیرند.[۴۰] وقتی که شهاب‌وار وارد جو زمین می‌شود، گرم می‌شود و نور رشته‌ای مانندی از آن دیده می‌شود که شهاب نام دارد.[۴۱] اما گاهی اوقات شهاب‌وارها از جو زمین می‌گذرند و بر روی زمین می‌افتند که این جسمی که بر روی زمین افتاده‌است را شهاب‌سنگ می‌نامند.[۴۲] دنباله‌دارهای مشهور[ویرایش]
ستارهٔ بیت‌اللحم[ویرایش] ستایش کودک توسط مغ. ستارهٔ بیت‌اللحم بالای سر کودک نشان داده شده‌است. این نقاشی توسط جوتو دی بوندوته کشیده شده‌است که او شاهد دنباله‌دار هالی در سال ۱۳۰۱ بوده‌است. ستارهٔ بیت‌اللحم یک پدیدهٔ آسمانی ذکرشده در انجیل متی و راهنمای سه مغ به زادگاه عیسی مسیح است. رویدادهای طبیعی نشان می‌دهد که ستارهٔ بیت‌اللحم می‌توانسته یک ابرنواختر، دنباله‌دار (دنباله‌دار هالی در ۱۱ یا ۱۲ سال پیش از میلاد قابل مشاهده بود)، شهاب‌سنگ یا مقارنهٔ سیاره‌ها بوده‌باشد. سال زایش مسیح نامشخص است، اما احتمالاً میان ۴ تا ۶ سال پیش از میلاد بوده‌است. کتاب مقدس می‌گوید که دو نفر این ستاره را دیده‌اند.[۵۷] آن سه مغ فرزانگانی از سرزمین پارس یا ایران و قادر به خواندن ستاره‌ها بودند.[۵۸] در اوایل سدهٔ هفدهم، یوهانس کپلر گفت که بیت‌اللحم ممکن‌است که یک نواختر باشد.[۵۷] به گفتهٔ کالین هامفریس در «ستارهٔ بیت‌اللحم –دنباله‌داری در ۵ سال پیش از میلاد– و زادروز عیسی» در مجلهٔ انجمن سلطنتی اخترشناسی در سال ۱۹۹۱، عیسی مسیح احتمالاً در پنج سال پیش از میلاد زاده شده‌است. در آن زمان، یک دنباله‌دار بزرگ، جدید و با حرکت آهسته به نام «سوئی-هزینگ» ثبت شده‌بود. هامفریس بر این باور است که این دنباله‌دار همان ستارهٔ بیت‌اللحم است.[۵۹] خرافات پیرامون دنباله‌دارها[ویرایش]دنباله‌دارها در بسیاری از فرهنگ‌های مختلف در سراسر جهان و در طول زمان از وحشت و ترس الهام گرفته شده‌اند. آن‌ها عناوینی هم‌چون «پیشروی حکم مجازات» و «تهدید گیتی» به خود گرفته‌اند. این اجرام هم‌چنین به عنوان پیشگویان فاجعه‌ها و پیامبران خدا در نظر گرفته می‌شدند. در دوران باستان، دنباله‌دارها قابل‌توجه‌ترین اشیاء در آسمان شب بودند. در بسیاری از فرهنگ‌ها، دنباله‌دارها حاملان پیام‌های خدایان هستند. برای نمونه، در برخی از فرهنگ‌ها، دم دنباله‌دارها ظاهر سر یک زن با موهای بلند پشت سرش است.[۲] جستارهای وابسته[ویرایش]پانویس[ویرایش]
پیوند به بیرون[ویرایش]
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Comets – nucleus, coma and tail:
A comet is an icy, small Solar System body that, when passing close to the Sun, warms and begins to release gases, a process called outgassing. This produces a visible atmosphere or coma, and sometimes also a tail. These phenomena are due to the effects of solar radiation and the solar wind acting upon the nucleus of the comet. Comet nuclei range from a few hundred meters to tens of kilometers across and are composed of loose collections of ice, dust, and small rocky particles. The coma may be up to 15 times Earth's diameter, while the tail may stretch one astronomical unit. If sufficiently bright, a comet may be seen from Earth without the aid of a telescope and may subtend an arc of 30° (60 Moons) across the sky. Comets have been observed and recorded since ancient times by many cultures. Comets usually have highly eccentric elliptical orbits, and they have a wide range of orbital periods, ranging from several years to potentially several millions of years. Short-period comets originate in the Kuiper belt or its associated scattered disc, which lie beyond the orbit of Neptune. Long-period comets are thought to originate in the Oort cloud, a spherical cloud of icy bodies extending from outside the Kuiper belt to halfway to the nearest star.[1] Long-period comets are set in motion towards the Sun from the Oort cloud by gravitational perturbations caused by passing stars and the galactic tide. Hyperbolic comets may pass once through the inner Solar System before being flung to interstellar space. The appearance of a comet is called an apparition. Comets are distinguished from asteroids by the presence of an extended, gravitationally unbound atmosphere surrounding their central nucleus. This atmosphere has parts termed the coma (the central part immediately surrounding the nucleus) and the tail (a typically linear section consisting of dust or gas blown out from the coma by the Sun's light pressure or outstreaming solar wind plasma). However, extinct comets that have passed close to the Sun many times have lost nearly all of their volatile ices and dust and may come to resemble small asteroids.[2] Asteroids are thought to have a different origin from comets, having formed inside the orbit of Jupiter rather than in the outer Solar System.[3][4] The discovery of main-belt comets and active centaur minor planets has blurred the distinction between asteroids and comets. In the early 21st century, the discovery of some minor bodies with long-period comet orbits, but characteristics of inner solar system asteroids, were called Manx comets. They are still classified as comets, such as C/2014 S3 (PANSTARRS).[5] 27 Manx comets were found from 2013 to 2017.[6] As of July 2019[update] there are 6,619 known comets,[7] a number that is steadily increasing as they are discovered. However, this represents only a tiny fraction of the total potential comet population, as the reservoir of comet-like bodies in the outer Solar System (in the Oort cloud) is estimated to be one trillion.[8][9] Roughly one comet per year is visible to the naked eye, though many of those are faint and unspectacular.[10] Particularly bright examples are called "great comets". Comets have been visited by unmanned probes such as the European Space Agency's Rosetta, which became the first to land a robotic spacecraft on a comet,[11] and NASA's Deep Impact, which blasted a crater on Comet Tempel 1 to study its interior. Etymology[edit].jpg) A comet was mentioned in the Anglo-Saxon Chronicle that allegedly made an appearance in 729 AD. The word comet derives from the Old English cometa from the Latin comēta or comētēs. That, in turn, is a latinization of the Greek κομήτης ("wearing long hair"), and the Oxford English Dictionary notes that the term (ἀστὴρ) κομήτης already meant "long-haired star, comet" in Greek. Κομήτης was derived from κομᾶν ("to wear the hair long"), which was itself derived from κόμη ("the hair of the head") and was used to mean "the tail of a comet".[12][13] The astronomical symbol for comets is Physical characteristics[edit]Nucleus[edit] Nucleus of 103P/Hartley as imaged during a spacecraft flyby. The nucleus is about 2 km in length. The solid, core structure of a comet is known as the nucleus. Cometary nuclei are composed of an amalgamation of rock, dust, water ice, and frozen carbon dioxide, carbon monoxide, methane, and ammonia.[15] As such, they are popularly described as "dirty snowballs" after Fred Whipple's model.[16] However, many comets have a higher dust content, leading them to be called "icy dirtballs".[17] Research conducted in 2014 suggests that comets are like "deep fried ice cream", in that their surfaces are formed of dense crystalline ice mixed with organic compounds, while the interior ice is colder and less dense.[18] The surface of the nucleus is generally dry, dusty or rocky, suggesting that the ices are hidden beneath a surface crust several metres thick. In addition to the gases already mentioned, the nuclei contain a variety of organic compounds, which may include methanol, hydrogen cyanide, formaldehyde, ethanol, and ethane and perhaps more complex molecules such as long-chain hydrocarbons and amino acids.[19][20] In 2009, it was confirmed that the amino acid glycine had been found in the comet dust recovered by NASA's Stardust mission.[21] In August 2011, a report, based on NASA studies of meteorites found on Earth, was published suggesting DNA and RNA components (adenine, guanine, and related organic molecules) may have been formed on asteroids and comets.[22][23]  Comet Borrelly exhibits jets, but has no surface ice. The outer surfaces of cometary nuclei have a very low albedo, making them among the least reflective objects found in the Solar System. The Giotto space probe found that the nucleus of Halley's Comet reflects about four percent of the light that falls on it,[24] and Deep Space 1 discovered that Comet Borrelly's surface reflects less than 3.0%;[24] by comparison, asphalt reflects seven percent. The dark surface material of the nucleus may consist of complex organic compounds. Solar heating drives off lighter volatile compounds, leaving behind larger organic compounds that tend to be very dark, like tar or crude oil. The low reflectivity of cometary surfaces causes them to absorb the heat that drives their outgassing processes.[25] Comet nuclei with radii of up to 30 kilometers (19 mi) have been observed,[26] but ascertaining their exact size is difficult.[27] The nucleus of 322P/SOHO is probably only 100–200 meters (330–660 ft) in diameter.[28] A lack of smaller comets being detected despite the increased sensitivity of instruments has led some to suggest that there is a real lack of comets smaller than 100 meters (330 ft) across.[29] Known comets have been estimated to have an average density of 0.6 g/cm3 (0.35 oz/cu in).[30] Because of their low mass, comet nuclei do not become spherical under their own gravity and therefore have irregular shapes.[31]  Comet 81P/Wild exhibits jets on light side and dark side, stark relief, and is dry. Roughly six percent of the near-Earth asteroids are thought to be extinct nuclei of comets that no longer experience outgassing,[32] including 14827 Hypnos and 3552 Don Quixote. Results from the Rosetta and Philae spacecraft show that the nucleus of 67P/Churyumov–Gerasimenko has no magnetic field, which suggests that magnetism may not have played a role in the early formation of planetesimals.[33][34] Further, the ALICE spectrograph on Rosetta determined that electrons (within 1 km (0.62 mi) above the comet nucleus) produced from photoionization of water molecules by solar radiation, and not photons from the Sun as thought earlier, are responsible for the degradation of water and carbon dioxide molecules released from the comet nucleus into its coma.[35][36] Instruments on the Philae lander found at least sixteen organic compounds at the comet's surface, four of which (acetamide, acetone, methyl isocyanate and propionaldehyde) have been detected for the first time on a comet.[37][38][39]
Coma[edit] The streams of dust and gas thus released form a huge and extremely thin atmosphere around the comet called the "coma". The force exerted on the coma by the Sun's radiation pressure and solar wind cause an enormous "tail" to form pointing away from the Sun.[48] The coma is generally made of H Although the solid nucleus of comets is generally less than 60 kilometers (37 mi) across, the coma may be thousands or millions of kilometers across, sometimes becoming larger than the Sun.[51] For example, about a month after an outburst in October 2007, comet 17P/Holmes briefly had a tenuous dust atmosphere larger than the Sun.[52] The Great Comet of 1811 also had a coma roughly the diameter of the Sun.[53] Even though the coma can become quite large, its size can decrease about the time it crosses the orbit of Mars around 1.5 astronomical units (220,000,000 km; 140,000,000 mi) from the Sun.[53] At this distance the solar wind becomes strong enough to blow the gas and dust away from the coma, and in doing so enlarging the tail.[53] Ion tails have been observed to extend one astronomical unit (150 million km) or more.[52] Both the coma and tail are illuminated by the Sun and may become visible when a comet passes through the inner Solar System, the dust reflects sunlight directly while the gases glow from ionisation.[54] Most comets are too faint to be visible without the aid of a telescope, but a few each decade become bright enough to be visible to the naked eye.[55] Occasionally a comet may experience a huge and sudden outburst of gas and dust, during which the size of the coma greatly increases for a period of time. This happened in 2007 to Comet Holmes.[56] In 1996, comets were found to emit X-rays.[57] This greatly surprised astronomers because X-ray emission is usually associated with very high-temperature bodies. The X-rays are generated by the interaction between comets and the solar wind: when highly charged solar wind ions fly through a cometary atmosphere, they collide with cometary atoms and molecules, "stealing" one or more electrons from the atom in a process called "charge exchange". This exchange or transfer of an electron to the solar wind ion is followed by its de-excitation into the ground state of the ion by the emission of X-rays and far ultraviolet photons.[58] Bow shock[edit]Bow shocks form as a result of the interaction between the solar wind and the cometary ionosphere, which is created by ionization of gases in the coma. As the comet approaches the Sun, increasing outgassing rates cause the coma to expand, and the sunlight ionizes gases in the coma. When the solar wind passes through this ion coma, the bow shock appears. The first observations were made in the 1980s and 90s as several spacecraft flew by comets 21P/Giacobini–Zinner,[59] 1P/Halley,[60] and 26P/Grigg–Skjellerup.[61] It was then found that the bow shocks at comets are wider and more gradual than the sharp planetary bow shocks seen at, for example, Earth. These observations were all made near perihelion when the bow shocks already were fully developed. The Rosetta spacecraft observed the bow shock at comet 67P/Churyumov–Gerasimenko at an early stage of bow shock development when the outgassing increased during the comet's journey toward the Sun. This young bow shock was called the "infant bow shock". The infant bow shock is asymmetric and, relative to the distance to the nucleus, wider than fully developed bow shocks.[62] Tails[edit]In the outer Solar System, comets remain frozen and inactive and are extremely difficult or impossible to detect from Earth due to their small size. Statistical detections of inactive comet nuclei in the Kuiper belt have been reported from observations by the Hubble Space Telescope[63][64] but these detections have been questioned.[65][66] As a comet approaches the inner Solar System, solar radiation causes the volatile materials within the comet to vaporize and stream out of the nucleus, carrying dust away with them. The streams of dust and gas each form their own distinct tail, pointing in slightly different directions. The tail of dust is left behind in the comet's orbit in such a manner that it often forms a curved tail called the type II or dust tail.[54] At the same time, the ion or type I tail, made of gases, always points directly away from the Sun because this gas is more strongly affected by the solar wind than is dust, following magnetic field lines rather than an orbital trajectory.[67] On occasions—such as when Earth passes through a comet's orbital plane, the antitail, pointing in the opposite direction to the ion and dust tails, may be seen.[68]  Diagram of a comet showing the dust trail, the dust tail, and the ion gas tail formed by solar wind. The observation of antitails contributed significantly to the discovery of solar wind.[69] The ion tail is formed as a result of the ionization by solar ultra-violet radiation of particles in the coma. Once the particles have been ionized, they attain a net positive electrical charge, which in turn gives rise to an "induced magnetosphere" around the comet. The comet and its induced magnetic field form an obstacle to outward flowing solar wind particles. Because the relative orbital speed of the comet and the solar wind is supersonic, a bow shock is formed upstream of the comet in the flow direction of the solar wind. In this bow shock, large concentrations of cometary ions (called "pick-up ions") congregate and act to "load" the solar magnetic field with plasma, such that the field lines "drape" around the comet forming the ion tail.[70] If the ion tail loading is sufficient, the magnetic field lines are squeezed together to the point where, at some distance along the ion tail, magnetic reconnection occurs. This leads to a "tail disconnection event".[70] This has been observed on a number of occasions, one notable event being recorded on 20 April 2007, when the ion tail of Encke's Comet was completely severed while the comet passed through a coronal mass ejection. This event was observed by the STEREO space probe.[71] In 2013, ESA scientists reported that the ionosphere of the planet Venus streams outwards in a manner similar to the ion tail seen streaming from a comet under similar conditions."[72][73] Jets[edit] Gas and snow jets of 103P/Hartley Uneven heating can cause newly generated gases to break out of a weak spot on the surface of comet's nucleus, like a geyser.[74] These streams of gas and dust can cause the nucleus to spin, and even split apart.[74] In 2010 it was revealed dry ice (frozen carbon dioxide) can power jets of material flowing out of a comet nucleus.[75] Infrared imaging of Hartley 2 shows such jets exiting and carrying with it dust grains into the coma.[76] Orbital characteristics[edit]Most comets are small Solar System bodies with elongated elliptical orbits that take them close to the Sun for a part of their orbit and then out into the further reaches of the Solar System for the remainder.[77] Comets are often classified according to the length of their orbital periods: The longer the period the more elongated the ellipse. Short period[edit]Periodic comets or short-period comets are generally defined as those having orbital periods of less than 200 years.[78] They usually orbit more-or-less in the ecliptic plane in the same direction as the planets.[79] Their orbits typically take them out to the region of the outer planets (Jupiter and beyond) at aphelion; for example, the aphelion of Halley's Comet is a little beyond the orbit of Neptune. Comets whose aphelia are near a major planet's orbit are called its "family".[80] Such families are thought to arise from the planet capturing formerly long-period comets into shorter orbits.[81] At the shorter orbital period extreme, Encke's Comet has an orbit that does not reach the orbit of Jupiter, and is known as an Encke-type comet. Short-period comets with orbital periods less than 20 years and low inclinations (up to 30 degrees) to the ecliptic are called traditional Jupiter-family comets (JFCs).[82][83] Those like Halley, with orbital periods of between 20 and 200 years and inclinations extending from zero to more than 90 degrees, are called Halley-type comets (HTCs).[84][85] As of 2019[update], 89 HTCs have been observed,[86] compared with 676 identified JFCs.[87] Recently discovered main-belt comets form a distinct class, orbiting in more circular orbits within the asteroid belt.[88] Because their elliptical orbits frequently take them close to the giant planets, comets are subject to further gravitational perturbations.[89] Short-period comets have a tendency for their aphelia to coincide with a giant planet's semi-major axis, with the JFCs being the largest group.[83] It is clear that comets coming in from the Oort cloud often have their orbits strongly influenced by the gravity of giant planets as a result of a close encounter. Jupiter is the source of the greatest perturbations, being more than twice as massive as all the other planets combined. These perturbations can deflect long-period comets into shorter orbital periods.[90][91] Based on their orbital characteristics, short-period comets are thought to originate from the centaurs and the Kuiper belt/scattered disc[92] —a disk of objects in the trans-Neptunian region—whereas the source of long-period comets is thought to be the far more distant spherical Oort cloud (after the Dutch astronomer Jan Hendrik Oort who hypothesized its existence).[93] Vast swarms of comet-like bodies are thought to orbit the Sun in these distant regions in roughly circular orbits. Occasionally the gravitational influence of the outer planets (in the case of Kuiper belt objects) or nearby stars (in the case of Oort cloud objects) may throw one of these bodies into an elliptical orbit that takes it inwards toward the Sun to form a visible comet. Unlike the return of periodic comets, whose orbits have been established by previous observations, the appearance of new comets by this mechanism is unpredictable.[94] Long period[edit] Orbits of Comet Kohoutek (red) and Earth (blue), illustrating the high eccentricity of its orbit and its rapid motion when close to the Sun. Long-period comets have highly eccentric orbits and periods ranging from 200 years to thousands of years.[95] An eccentricity greater than 1 when near perihelion does not necessarily mean that a comet will leave the Solar System.[96] For example, Comet McNaught had a heliocentric osculating eccentricity of 1.000019 near its perihelion passage epoch in January 2007 but is bound to the Sun with roughly a 92,600-year orbit because the eccentricity drops below 1 as it moves farther from the Sun. The future orbit of a long-period comet is properly obtained when the osculating orbit is computed at an epoch after leaving the planetary region and is calculated with respect to the center of mass of the Solar System. By definition long-period comets remain gravitationally bound to the Sun; those comets that are ejected from the Solar System due to close passes by major planets are no longer properly considered as having "periods". The orbits of long-period comets take them far beyond the outer planets at aphelia, and the plane of their orbits need not lie near the ecliptic. Long-period comets such as Comet West and C/1999 F1 can have aphelion distances of nearly 70,000 AU with orbital periods estimated around 6 million years. Single-apparition or non-periodic comets are similar to long-period comets because they also have parabolic or slightly hyperbolic trajectories[95] when near perihelion in the inner Solar System. However, gravitational perturbations from giant planets cause their orbits to change. Single-apparition comets have a hyperbolic or parabolic osculating orbit which allows them to permanently exit the Solar System after a single pass of the Sun.[97] The Sun's Hill sphere has an unstable maximum boundary of 230,000 AU (1.1 pc; 3.6 ly).[98] Only a few hundred comets have been seen to reach a hyperbolic orbit (e > 1) when near perihelion[99] that using a heliocentric unperturbed two-body best-fit suggests they may escape the Solar System. As of 2019[update], only two objects have been discovered with an eccentricity significantly greater than one: 1I/ʻOumuamua and 2I/Borisov, indicating an origin outside the Solar System. While ʻOumuamua, with an eccentrcity of about 1.2, showed no optical signs of cometary activity during its passage through the inner Solar System in October 2017, changes to its trajectory—which suggests outgassing—indicate that it is probably a comet.[100] On the other hand, 2I/Borisov, with an estimated eccentricity of about 3.36, has been observed to have the coma feature of comets, and is considered the first detected interstellar comet.[101][102] Comet C/1980 E1 had an orbital period of roughly 7.1 million years before the 1982 perihelion passage, but a 1980 encounter with Jupiter accelerated the comet giving it the largest eccentricity (1.057) of any known hyperbolic comet.[103] Comets not expected to return to the inner Solar System include C/1980 E1, C/2000 U5, C/2001 Q4 (NEAT), C/2009 R1, C/1956 R1, and C/2007 F1 (LONEOS). Some authorities use the term "periodic comet" to refer to any comet with a periodic orbit (that is, all short-period comets plus all long-period comets),[104] whereas others use it to mean exclusively short-period comets.[95] Similarly, although the literal meaning of "non-periodic comet" is the same as "single-apparition comet", some use it to mean all comets that are not "periodic" in the second sense (that is, to also include all comets with a period greater than 200 years). Early observations have revealed a few genuinely hyperbolic (i.e. non-periodic) trajectories, but no more than could be accounted for by perturbations from Jupiter. If comets pervaded interstellar space, they would be moving with velocities of the same order as the relative velocities of stars near the Sun (a few tens of km per second). If such objects entered the Solar System, they would have positive specific orbital energy and would be observed to have genuinely hyperbolic trajectories. A rough calculation shows that there might be four hyperbolic comets per century within Jupiter's orbit, give or take one and perhaps two orders of magnitude.[105]
Oort cloud and Hills cloud[edit] The Oort cloud is thought to occupy a vast space starting from between 2,000 and 5,000 AU (0.03 and 0.08 ly)[107] to as far as 50,000 AU (0.79 ly)[84] from the Sun. Some estimates place the outer edge at between 100,000 and 200,000 AU (1.58 and 3.16 ly).[107] The region can be subdivided into a spherical outer Oort cloud of 20,000–50,000 AU (0.32–0.79 ly), and a doughnut-shaped inner cloud, the Hills cloud, of 2,000–20,000 AU (0.03–0.32 ly).[108] The outer cloud is only weakly bound to the Sun and supplies the long-period (and possibly Halley-type) comets that fall to inside the orbit of Neptune.[84] The inner Oort cloud is also known as the Hills cloud, named after J. G. Hills, who proposed its existence in 1981.[109] Models predict that the inner cloud should have tens or hundreds of times as many cometary nuclei as the outer halo;[109][110][111] it is seen as a possible source of new comets that resupply the relatively tenuous outer cloud as the latter's numbers are gradually depleted. The Hills cloud explains the continued existence of the Oort cloud after billions of years.[112] Exocomets[edit]Exocomets beyond the Solar System have also been detected and may be common in the Milky Way.[113] The first exocomet system detected was around Beta Pictoris, a very young A-type main-sequence star, in 1987.[114][115] A total of 10 such exocomet systems have been identified as of 2013[update], using the absorption spectrum caused by the large clouds of gas emitted by comets when passing close to their star.[113][114] Effects of comets[edit] Diagram of Perseids meteors Connection to meteor showers[edit]As a comet is heated during close passes to the Sun, outgassing of its icy components also releases solid debris too large to be swept away by radiation pressure and the solar wind.[116] If Earth's orbit sends it through that trail of debris, which is composed mostly of fine grains of rocky material, there is likely to be a meteor shower as Earth passes through. Denser trails of debris produce quick but intense meteor showers and less dense trails create longer but less intense showers. Typically, the density of the debris trail is related to how long ago the parent comet released the material.[117][118] The Perseid meteor shower, for example, occurs every year between 9 and 13 August, when Earth passes through the orbit of Comet Swift–Tuttle. Halley's Comet is the source of the Orionid shower in October.[119][120] Comets and impact on life[edit]Many comets and asteroids collided with Earth in its early stages. Many scientists think that comets bombarding the young Earth about 4 billion years ago brought the vast quantities of water that now fill Earth's oceans, or at least a significant portion of it. Others have cast doubt on this idea.[121] The detection of organic molecules, including polycyclic aromatic hydrocarbons,[18] in significant quantities in comets has led to speculation that comets or meteorites may have brought the precursors of life—or even life itself—to Earth.[122] In 2013 it was suggested that impacts between rocky and icy surfaces, such as comets, had the potential to create the amino acids that make up proteins through shock synthesis.[123] In 2015, scientists found significant amounts of molecular oxygen in the outgassings of comet 67P, suggesting that the molecule may occur more often than had been thought, and thus less an indicator of life as has been supposed.[124] It is suspected that comet impacts have, over long timescales, also delivered significant quantities of water to Earth's Moon, some of which may have survived as lunar ice.[125] Comet and meteoroid impacts are also thought to be responsible for the existence of tektites and australites.[126] Fear of comets[edit]Fear of comets as acts of God and signs of impending doom was highest in Europe from AD 1200 to 1650.[127] The year after the Great Comet of 1618, for example, Gotthard Arthusius published a pamphlet stating that it was a sign that the Day of Judgment was near.[128] He listed ten pages of comet-related disasters, including "earthquakes, floods, changes in river courses, hail storms, hot and dry weather, poor harvests, epidemics, war and treason and high prices". By 1700 most scholars concluded that such events occurred whether a comet was seen or not. Using Edmund Halley's records of comet sightings, however, William Whiston in 1711 wrote that the Great Comet of 1680 had a periodicity of 574 years and was responsible for the worldwide flood in the Book of Genesis, by pouring water on Earth. His announcement revived for another century fear of comets, now as direct threats to the world instead of signs of disasters.[127] Spectroscopic analysis in 1910 found the toxic gas cyanogen in the tail of Halley's Comet,[129] causing panicked buying of gas masks and quack "anti-comet pills" and "anti-comet umbrellas" by the public.[130] Fate of comets[edit]Departure (ejection) from Solar System[edit]If a comet is traveling fast enough, it may leave the Solar System. Such comets follow the open path of a hyperbola, and as such they are called hyperbolic comets. To date, comets are only known to be ejected by interacting with another object in the Solar System, such as Jupiter.[131] An example of this is thought to be Comet C/1980 E1, which was shifted from a predicted orbit of 7.1 million years around the Sun, to a hyperbolic trajectory, after a 1980 close pass by the planet Jupiter.[132] Volatiles exhausted[edit]Jupiter-family comets and long-period comets appear to follow very different fading laws. The JFCs are active over a lifetime of about 10,000 years or ~1,000 orbits whereas long-period comets fade much faster. Only 10% of the long-period comets survive more than 50 passages to small perihelion and only 1% of them survive more than 2,000 passages.[32] Eventually most of the volatile material contained in a comet nucleus evaporates, and the comet becomes a small, dark, inert lump of rock or rubble that can resemble an asteroid.[133] Some asteroids in elliptical orbits are now identified as extinct comets.[134][135][136][137] Roughly six percent of the near-Earth asteroids are thought to be extinct comet nuclei.[32] Breakup and collisions[edit]The nucleus of some comets may be fragile, a conclusion supported by the observation of comets splitting apart.[138] A significant cometary disruption was that of Comet Shoemaker–Levy 9, which was discovered in 1993. A close encounter in July 1992 had broken it into pieces, and over a period of six days in July 1994, these pieces fell into Jupiter's atmosphere—the first time astronomers had observed a collision between two objects in the Solar System.[139][140] Other splitting comets include 3D/Biela in 1846 and 73P/Schwassmann–Wachmann from 1995 to 2006.[141] Greek historian Ephorus reported that a comet split apart as far back as the winter of 372–373 BC.[142] Comets are suspected of splitting due to thermal stress, internal gas pressure, or impact.[143] Comets 42P/Neujmin and 53P/Van Biesbroeck appear to be fragments of a parent comet. Numerical integrations have shown that both comets had a rather close approach to Jupiter in January 1850, and that, before 1850, the two orbits were nearly identical.[144] Some comets have been observed to break up during their perihelion passage, including great comets West and Ikeya–Seki. Biela's Comet was one significant example, when it broke into two pieces during its passage through the perihelion in 1846. These two comets were seen separately in 1852, but never again afterward. Instead, spectacular meteor showers were seen in 1872 and 1885 when the comet should have been visible. A minor meteor shower, the Andromedids, occurs annually in November, and it is caused when Earth crosses the orbit of Biela's Comet.[145] Some comets meet a more spectacular end – either falling into the Sun[146] or smashing into a planet or other body. Collisions between comets and planets or moons were common in the early Solar System: some of the many craters on the Moon, for example, may have been caused by comets. A recent collision of a comet with a planet occurred in July 1994 when Comet Shoemaker–Levy 9 broke up into pieces and collided with Jupiter.[147] Brown spots mark impact sites of Comet Shoemaker–Levy 9 on Jupiter The break up of 73P/Schwassmann–Wachmann within three days (1995) Ghost tail of C/2015 D1 (SOHO) after passage at the Sun Nomenclature[edit] Halley's Comet in 1910 The names given to comets have followed several different conventions over the past two centuries. Prior to the early 20th century, most comets were simply referred to by the year when they appeared, sometimes with additional adjectives for particularly bright comets; thus, the "Great Comet of 1680", the "Great Comet of 1882", and the "Great January Comet of 1910". After Edmund Halley demonstrated that the comets of 1531, 1607, and 1682 were the same body and successfully predicted its return in 1759 by calculating its orbit, that comet became known as Halley's Comet.[149] Similarly, the second and third known periodic comets, Encke's Comet[150] and Biela's Comet,[151] were named after the astronomers who calculated their orbits rather than their original discoverers. Later, periodic comets were usually named after their discoverers, but comets that had appeared only once continued to be referred to by the year of their appearance.[152] In the early 20th century, the convention of naming comets after their discoverers became common, and this remains so today. A comet can be named after its discoverers, or an instrument or program that helped to find it.[152] History of study[edit]Early observations and thought[edit] Halley's Comet appeared in 1066, prior to the Battle of Hastings, and is depicted in the Bayeux Tapestry. From ancient sources, such as Chinese oracle bones, it is known that comets have been noticed by humans for millennia.[153] Until the sixteenth century, comets were usually considered bad omens of deaths of kings or noble men, or coming catastrophes, or even interpreted as attacks by heavenly beings against terrestrial inhabitants.[154][155] Aristotle was the first known scientist to utilize various theories and observational facts to employ a consistent, structured cosmological theory of comets. He believed that comets were atmospheric phenomena, due to the fact that they could appear outside of the Zodiac and vary in brightness over the course of a few days. Aristotle's cometary theory arose from his observations and cosmological theory that everything in the cosmos is arranged in a distinct configuration.[156] Seneca rejected Aristotle's views and thought comets to be more permanent than suggested by their brief flashes across the sky.[157] Pliny the Elder believed that comets were connected with political unrest and death.[158] Pliny observed comets as "human like", often describing their tails with "long hair" or "long beard" and used his descriptions to further his classifications.[159] In India, by the 6th century astronomers believed that comets were celestial bodies that re-appeared periodically. This was the view expressed in the 6th century by the astronomers Varāhamihira and Bhadrabahu, and the 10th-century astronomer Bhaṭṭotpala listed the names and estimated periods of certain comets, but it is not known how these figures were calculated or how accurate they were.[160] In the 16th century Tycho Brahe demonstrated that comets must exist outside Earth's atmosphere by measuring the parallax of the Great Comet of 1577 from observations collected by geographically separated observers. Within the precision of the measurements, this implied the comet must be at least four times more distant than from Earth to the Moon.[161][162] Based on observations in 1664, Giovanni Borelli recorded the longitudes and latitudes of comets that he observed, and suggested that cometary orbits may be parabolic.[163] Orbital studies[edit]Isaac Newton, in his Principia Mathematica of 1687, proved that an object moving under the influence of gravity must trace out an orbit shaped like one of the conic sections, and he demonstrated how to fit a comet's path through the sky to a parabolic orbit, using the comet of 1680 as an example.[164] In 1705, Edmond Halley (1656–1742) applied Newton's method to twenty-three cometary apparitions that had occurred between 1337 and 1698. He noted that three of these, the comets of 1531, 1607, and 1682, had very similar orbital elements, and he was further able to account for the slight differences in their orbits in terms of gravitational perturbation caused by Jupiter and Saturn. Confident that these three apparitions had been three appearances of the same comet, he predicted that it would appear again in 1758–9.[165] Halley's predicted return date was later refined by a team of three French mathematicians: Alexis Clairaut, Joseph Lalande, and Nicole-Reine Lepaute, who predicted the date of the comet's 1759 perihelion to within one month's accuracy.[166][167] When the comet returned as predicted, it became known as Halley's Comet (with the latter-day designation of 1P/Halley). It will next appear in 2061.[168] Studies of physical characteristics[edit]Isaac Newton described comets as compact and durable solid bodies moving in oblique orbit and their tails as thin streams of vapor emitted by their nuclei, ignited or heated by the Sun. Newton suspected that comets were the origin of the life-supporting component of air.[169] From his huge vapouring train perhaps to shake
Reviving moisture on the numerous orbs, Thro' which his long ellipsis winds; perhaps To lend new fuel to declining suns, To light up worlds, and feed th' ethereal fire. James Thomson The Seasons (1730; 1748)[170] As early as the 18th century, some scientists had made correct hypotheses as to comets' physical composition. In 1755, Immanuel Kant hypothesized that comets are composed of some volatile substance, whose vaporization gives rise to their brilliant displays near perihelion.[171] In 1836, the German mathematician Friedrich Wilhelm Bessel, after observing streams of vapor during the appearance of Halley's Comet in 1835, proposed that the jet forces of evaporating material could be great enough to significantly alter a comet's orbit, and he argued that the non-gravitational movements of Encke's Comet resulted from this phenomenon.[172] In 1950, Fred Lawrence Whipple proposed that rather than being rocky objects containing some ice, comets were icy objects containing some dust and rock.[173] This "dirty snowball" model soon became accepted and appeared to be supported by the observations of an armada of spacecraft (including the European Space Agency's Giotto probe and the Soviet Union's Vega 1 and Vega 2) that flew through the coma of Halley's Comet in 1986, photographed the nucleus, and observed jets of evaporating material.[174] On 22 January 2014, ESA scientists reported the detection, for the first definitive time, of water vapor on the dwarf planet Ceres, the largest object in the asteroid belt.[175] The detection was made by using the far-infrared abilities of the Herschel Space Observatory.[176] The finding is unexpected because comets, not asteroids, are typically considered to "sprout jets and plumes". According to one of the scientists, "The lines are becoming more and more blurred between comets and asteroids."[176] On 11 August 2014, astronomers released studies, using the Atacama Large Millimeter/Submillimeter Array (ALMA) for the first time, that detailed the distribution of HCN, HNC, H Spacecraft missions[edit]
Great comets[edit].png) Woodcut of the Great Comet of 1577 Approximately once a decade, a comet becomes bright enough to be noticed by a casual observer, leading such comets to be designated as great comets.[142] Predicting whether a comet will become a great comet is notoriously difficult, as many factors may cause a comet's brightness to depart drastically from predictions.[187] Broadly speaking, if a comet has a large and active nucleus, will pass close to the Sun, and is not obscured by the Sun as seen from Earth when at its brightest, it has a chance of becoming a great comet. However, Comet Kohoutek in 1973 fulfilled all the criteria and was expected to become spectacular but failed to do so.[188] Comet West, which appeared three years later, had much lower expectations but became an extremely impressive comet.[189] The Great Comet of 1577 is a well known example of a great comet. The Great Comet of 1577 passed near Earth as a non-periodic comet and was seen by many, including well-known astronomers Tycho Brahe and Taqi ad-Din. Observations of this comet led to several significant findings regarding cometary science, especially for Brahe. The late 20th century saw a lengthy gap without the appearance of any great comets, followed by the arrival of two in quick succession—Comet Hyakutake in 1996, followed by Hale–Bopp, which reached maximum brightness in 1997 having been discovered two years earlier. The first great comet of the 21st century was C/2006 P1 (McNaught), which became visible to naked eye observers in January 2007. It was the brightest in over 40 years.[190] Sungrazing comets[edit]A sungrazing comet is a comet that passes extremely close to the Sun at perihelion, generally within a few million kilometers.[191] Although small sungrazers can be completely evaporated during such a close approach to the Sun, larger sungrazers can survive many perihelion passages. However, the strong tidal forces they experience often lead to their fragmentation.[192] About 90% of the sungrazers observed with SOHO are members of the Kreutz group, which all originate from one giant comet that broke up into many smaller comets during its first passage through the inner Solar System.[193] The remainder contains some sporadic sungrazers, but four other related groups of comets have been identified among them: the Kracht, Kracht 2a, Marsden, and Meyer groups. The Marsden and Kracht groups both appear to be related to Comet 96P/Machholz, which is also the parent of two meteor streams, the Quadrantids and the Arietids.[194] Unusual comets[edit] Euler diagram showing the types of bodies in the Solar System. Of the thousands of known comets, some exhibit unusual properties. Comet Encke (2P/Encke) orbits from outside the asteroid belt to just inside the orbit of the planet Mercury whereas the Comet 29P/Schwassmann–Wachmann currently travels in a nearly circular orbit entirely between the orbits of Jupiter and Saturn.[195] 2060 Chiron, whose unstable orbit is between Saturn and Uranus, was originally classified as an asteroid until a faint coma was noticed.[196] Similarly, Comet Shoemaker–Levy 2 was originally designated asteroid 1990 UL3.[197] (See also Fate of comets, above) Centaurs[edit]Centaurs typically behave with characteristics of both asteroids and comets.[198] Centaurs can be classified as comets such as 60558 Echeclus, and 166P/NEAT. 166P/NEAT was discovered while it exhibited a coma, and so is classified as a comet despite its orbit, and 60558 Echeclus was discovered without a coma but later became active,[199] and was then classified as both a comet and an asteroid (174P/Echeclus). One plan for Cassini involved sending it to a centaur, but NASA decided to destroy it instead.[200] Observation[edit]A comet may be discovered photographically using a wide-field telescope or visually with binoculars. However, even without access to optical equipment, it is still possible for the amateur astronomer to discover a sungrazing comet online by downloading images accumulated by some satellite observatories such as SOHO.[201] SOHO's 2000th comet was discovered by Polish amateur astronomer Michał Kusiak on 26 December 2010[202] and both discoverers of Hale–Bopp used amateur equipment (although Hale was not an amateur). Lost[edit]A number of periodic comets discovered in earlier decades or previous centuries are now lost comets. Their orbits were never known well enough to predict future appearances or the comets have disintegrated. However, occasionally a "new" comet is discovered, and calculation of its orbit shows it to be an old "lost" comet. An example is Comet 11P/Tempel–Swift–LINEAR, discovered in 1869 but unobservable after 1908 because of perturbations by Jupiter. It was not found again until accidentally rediscovered by LINEAR in 2001.[203] There are at least 18 comets that fit this category.[204] In popular culture[edit]The depiction of comets in popular culture is firmly rooted in the long Western tradition of seeing comets as harbingers of doom and as omens of world-altering change.[205] Halley's Comet alone has caused a slew of sensationalist publications of all sorts at each of its reappearances. It was especially noted that the birth and death of some notable persons coincided with separate appearances of the comet, such as with writers Mark Twain (who correctly speculated that he'd "go out with the comet" in 1910)[205] and Eudora Welty, to whose life Mary Chapin Carpenter dedicated the song "Halley Came to Jackson".[205] In times past, bright comets often inspired panic and hysteria in the general population, being thought of as bad omens. More recently, during the passage of Halley's Comet in 1910, Earth passed through the comet's tail, and erroneous newspaper reports inspired a fear that cyanogen in the tail might poison millions,[206] whereas the appearance of Comet Hale–Bopp in 1997 triggered the mass suicide of the Heaven's Gate cult.[207] In science fiction, the impact of comets has been depicted as a threat overcome by technology and heroism (as in the 1998 films Deep Impact and Armageddon), or as a trigger of global apocalypse (Lucifer's Hammer, 1979) or zombies (Night of the Comet, 1984).[205] In Jules Verne's Off on a Comet a group of people are stranded on a comet orbiting the Sun, while a large manned space expedition visits Halley's Comet in Sir Arthur C. Clarke's novel 2061: Odyssey Three.[208] Gallery[edit]
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