Free Astronomy Magazine November-December 2023 ARABIC VERSION

N 35 ASA’s James Webb Space Telescope’s high resolu- tion, near-infrared look at Her- big-Haro 211 reveals exquisite detail of the outflow of a young star, an infantile ana- logue of our Sun. Herbig-Haro objects are formed when stellar winds or jets of gas spewing from newborn stars form shock waves colliding with nearby gas and dust at high speeds. The image showcases a series of bow shocks to the southeast (lower-left) and northwest (upper-right) as well as the narrow bipolar jet that powers them in unprecedented detail. Molecules excited by the turbu- lent conditions, including mo- lecular hydrogen, carbon monoxide and silicon monox- ide, emit infrared light, col- lected by Webb, that map out the structure of the outflows. [ESA/Webb, NASA, CSA, Tom Ray (Dublin)] Molecules excited by the turbulent conditions, including molecular hy- drogen, carbon monoxide, and sili- con monoxide, emit infrared light that Webb can collect to map out the structure of the outflows. The image showcases a series of bow shocks to the southeast (lower- left) and northwest (upper-right) as well as the narrow bipolar jet that powers them. Webb reveals this scene in unprecedented detail — roughly 5 to 10 times higher spatial resolution than any previous images of HH 211. The inner jet is seen to “wiggle” with mirror symmetry on either side of the central protostar. This is in agreement with observa- tions on smaller scales and suggests that the protostar may in fact be an unresolved binary star. Earlier observations of HH 211 with ground-based telescopes revealed giant bow shocks moving away from us (northwest) and moving to- wards us (southeast) and cavity-like structures in shocked hydrogen and carbon monoxide respectively, as well as a knotty and wiggling bipo- lar jet in silicon monoxide. Researchers have used Webb’s new observations to determine that the object’s outflow is relatively slow in comparison to more evolved proto- stars with similar types of outflows. The team measured the velocities of the innermost outflow structures to be roughly 48-60 miles per second (80 to 100 kilometers per second). However, the difference in velocity between these sections of the out- flow and the leading material they’re colliding with — the shock wave — is much smaller. The re- searchers concluded that outflows from the youngest stars, like that in the center of HH 211, are mostly made up of molecules, because the comparatively low shock wave ve- locities are not energetic enough to break the molecules apart into sim- pler atoms and ions.  ــﺐ ــﺔ ﻟﺘﻠﺴــ ﻮبﺟــ ﻤﺲو اﻟﺪﻗــﺔ اﻟﻌﺎﻟ اﻟﻔﻀـﺎﺋﻲاﻟﺘــﺎﺑﻊ ﻟـــ ASA إن اﻟﻨﻈـﺮة ـﺔ ﻣـﻦ اﻷﺷــﻌﺔ ﺗﺤـﺖ ا ﻤـﺮاء إﻟــﻰ اﻟﻘﺮ ـــــــــــــﻴـﺞ ــــــــــــﻢﻫ ﻧ - ﻫـــــــــــــﺎرو 211 ﺗﻜﺸـــــــــــــﻒ ــــﻢﺷــــﺎب ﺗﻔﺎﺻــــﻴﻞ راﺋﻌــــﺔ ﻋــــﻦ ﺗــــﺪﻓﻖ ﻧ إﻟــــــــﻰاﻟــــــــ ـ ﺨﺎرج وﻫــــــــﻮ ﻧﻈــــــــ ﻃﻔـــــــــﻮﻟﻲ ﻟﺸﻤﺴﻨﺎ . ــﻴـﺞ ﺗﺘﺸـــ ﻞ أﺟﺴـــﺎمﻫ - ﻫـــﺎرو ﻋﻨـــﺪﻣﺎ ــﺔ أو ﻧﻔﺎﺛــ ﺗﺸـ ﻞ اﻟﺮ ــﺎح اﻟﻨ ﻤ ﺎت اﻟﻐــﺎز اﻟﻤﻨ ﻌﺜــــﺔ ﻣــــﻦ اﻟﻨﺠــــﻮمﺣﺪ ﺜــــﺔ اﻟــــﻮﻻدة ﻣﻮﺟـــــــــــﺎتﺻـــــــــــﺪﻣ ﺔ ﺗﺼـــــــــــﻄﺪم ﺎﻟﻐـــــــــــﺎز ـــــــــــﺔ ـــــــــــﺎراﻟﻘﺮ ـــــــــــﺐ ﺴـــــــــــﺮﻋﺎتﻋﺎﻟ واﻟﻐ . ﺗﻌـﺮضاﻟﺼــﻮرةﺳﻠﺴــﻠﺔ ﻣــﻦ اﻟﺼــﺪﻣﺎت اﻟﻘﻮﺳــــــ ﺔ ﺎﺗﺠــــــﺎﻩ اﻟــــــ ـ ﺠﻨﻮب اﻟﺸـــــــﺮﻗﻲ ) أﺳــــــﻔﻞ اﻟ ﺴــــــﺎر ( واﻟﺸــــــﻤﺎل اﻟﻐﺮ ــــــﻲ ) أﻋﻠـــﻰاﻟ ﻤــــ ( ــــﺎر ﺎﻹﺿـــﺎﻓﺔ إﻟــــﻰاﻟﺘ ﻳﺰودﻫــــﺎ اﻟﻀــــﻴﻖ ﺛﻨــــﺎﺋﻲاﻟﻘﻄــــﺐ اﻟــــﺬ ﺎﻟﻄﺎﻗـــــﺔ ﺘﻔﺎﺻـــــﻴﻞ ﻏـــــ ﻣﺴـــــﺒﻮﻗﺔ إن . ـ اﻟـــــــــــــ ﺗﺜ ﻫـــــــــــــﺎ اﻟﻈــــــــــــــﺮوف ﺠﺰ ﺌﺎت اﻟـــــــــــــ ـﺪروﺟ اﻟﻤﻀﻄﺮ ﺔ، ﻤﺎ ﻓﻲذﻟـﻚ اﻟﻬ ـ اﻟـــــــ وأول أﻛﺴـــــــ ﺪ اﻟﻜﺮ ـــــــﻮن ﺠﺰ وأول أﻛﺴ ﺪ اﻟﺴ ﻠﻴ ﻮن ﺗ ﻌﺚﺿﻮء اﻷﺷﻌﺔ ﺗﺤـــﺖ اﻟـــ ـ ﻳ ﻤﻌـــﮫ ﻤﺮاء اﻟـــﺬ ﺗﻠﺴـــ ﻮب ـــــــــﺔ ﻳﺮﺳــــــــﻢﺧﺮ ﻄـــــــــﺔ ﻟ ﻨ ــــــــﺐواﻟـــــــــﺬ و اﻟﺘﺪﻓﻘﺎت اﻟـﺨﺎرﺟ ﺔ . 35 إن اﻟﺠﺰﻳ ﺌــﺎت اﻟﺘــﻲ ﺗﺜ ﻫــﺎ اﻟ ﻈــﺮوف ا ﻀﻄﺮﺑﺔ ﺑﻤﺎ ﰲ ذﻟﻚ اﻟﻬﻴﺪروﺟ اﻟﺠﺰﻳﺌﻲ وأول أﻛﺴـــﻴﺪ اﻟﻜﺮﺑـــﻮن وأول أﻛﺴـــﻴﺪ اﻟﺴﻴﻠﻴﻜﻮن ﻳ ﻨﺒﻌﺚ ﻣﻨﻬ ﺎ ﺿﻮء اﻷﺷﻌﺔ ﺗﺤﺖ اﻟﺤﻤﺮاء اﻟـﺬي ﻳﺴـﺘﻄﻴﻊ ﺗﻠﺴـﻜﻮب وﻳـﺐ ﺟﻤﻌـﻪ ﻟﺮﺳـﻢ ﺧﺮﻳﻄـﺔ ﻟﺒﻨﻴـﺔ اﻟﺘـﺪﻓﻘﺎت اﻟﺨﺎرﺟﻴﺔ . ﺗﻌـﺮض اﻟﺼـﻮرة ﺳﻠﺴـﻠﺔ ﻣـﻦ اﻟﺼﺪﻣﺎت اﻟﻘﻮﺳﻴﺔ ﺑﺎﺗﺠﺎه اﻟﺠﻨﻮب اﻟﴩﻗﻲ ) أﺳﻔﻞ ﻟﻴﻤ واﻟ ( ﺸـﻤﺎل اﻟــﴩﻗﻲ أﻋـﲆ ) اﻟﻴﺴﺎر ( ﺑﺎﻹﺿﺎﻓﺔ إﱃ اﻟﺘﻴﺎر اﻟﻀـﻴﻖ ﺛﻨـﺎﺋﻲ اﻟﻘﻄﺐ اﻟـﺬي ﻳﺰودﻫـﺎ ﺑﺎﻟﻄﺎﻗـﺔ . ﻳﻜﺸـﻒ ﺗﻠﺴﻜﻮب وﻳﺐ ﻋﻦ ﻫـﺬا ا ﺸـﻬﺪ ﺑﺘﻔﺎﺻـﻴﻞ ﻏ ﻣﺴﺒﻮﻗﺔ ﺑ ﺪﻗﺔ ﻣﻜﺎﻧﻴﺔ أﻋﲆ ﺑﺤﻮاﱄ 5 إﱃ 10 ﻣﺮات ﻣﻦ أي ﺻﻮر ﻟـ HH 211 ﻳُﻨﻈـﺮ إﱃ اﻟﺘﺪﻓﻖ اﻟﺪاﺧﲇ ﻋـﲆ أﻧـﻪ ﻳﻬﺘـﺰ " ﻣـﻊ " ﺗﻨﺎﻇﺮ ا ﺮآة ﻋﲆ ﺟﺎ ﻧﺒﻲ اﻟﻨﺠﻢ اﻷوﱄ ا ﺮﻛﺰي وﻫﺬا ﻳﺘﻔـﻖ ﻣـﻊ اﻷرﺻـﺎد ﻋـﲆ ا ﻘـﺎﻳﻴﺲ اﻷﺻﻐﺮ وﻳﺸ إﱃ أن اﻟﻨﺠﻢ اﻷوﱄ ﻗﺪ ﻳ ﻜﻮن ﰲ اﻟﻮاﻗﻊ ﻧﺠﻤ ﺎً ﺛﻨﺎﺋﻴﺎً ﻟـﻢ ﻳـﺘﻢ ﺣﻠـﻪ ﺑﻌـﺪ . ﻛﺸـﻔﺖ اﻷ رﺻـﺎد اﻟﺴـﺎﺑﻘﺔ ﻟــ HH 211 ﺑﺎﺳــﺘﺨﺪام اﻟﺘﻠﺴــﻜﻮﺑﺎت اﻷرﺿــﻴﺔ ﻋــ ﻦ ﺻﺪﻣﺎت ﻗﻮﺳﻴﺔ ﻋﻤﻼﻗﺔ ﺗﺘﺤﺮك ﺑﻌﻴﺪ اً ﻋﻨـﺎ ) ( ﴍق ﺷـﻤﺎل وﺗﺘﺤـﺮك ﻧﺤﻮﻧـﺎ ) ﺟﻨـﻮب ( ﻏــﺮب وﻫﻴﺎﻛــﻞ ﺗﺸــﺒﻪ اﻟﺘﺠﻮﻳــﻒ ﰲ اﻟﻬﻴـــﺪروﺟ وأول أﻛﺴـــﻴ ﺪ اﻟﻜﺮﺑـــﻮن ا ﺼﺪوﻣ ﻋﲆ اﻟﺘﻮاﱄ ﺑﺎﻹﺿـﺎﻓﺔ إﱃ ﻧﻔﺎﺛـﺔ ﺛﻨﺎﺋﻴﺔ اﻟﻘﻄـﺐ ﻣﻌﻘـﻮدة وﻣﺘﺬﺑﺬﺑـﺔ ﰲ أول أﻛﺴـﻴﺪ اﻟﺴـﻴﻠﻴﻜﻮ .ن اﺳـﺘﺨﺪم اﻟﺒـﺎﺣﺜﻮن أرﺻﺎد ﺗﻠﺴﻜﻮب وﻳﺐ اﻟﺠﺪﻳـﺪة ﻟﺘﺤﺪﻳـﺪ أن اﻟﺘﺪﻓﻖ اﻟﺨـﺎرﺟﻲ ﻟﻠﺠﺴـﻢ ﺑﻄـﻲء ﻧﺴـﺒﻴ ﺎً رﻧﺔ ﺑ ﻣﻘﺎ ﺎﻟﻨﺠﻮم اﻷوﻟﻴﺔ اﻷﻛﺜﺮ ﺗﻄﻮر اً واﻟﺘﻲ ﻟﻬﺎ أﻧﻮاع ﻣﻤﺎﺛﻠﺔ ﻣﻦ اﻟﺘﺪﻓﻘﺎت اﻟﺨﺎرﺟﻴﺔ . ﻗﺎم اﻟﻔﺮﻳﻖ ﺑﻘﻴﺎسﴎﻋﺎت ﻫﻴﺎﻛﻞ اﻟﺘـﺪﻓﻖ اﻟﺨﺎرﺟﻲ اﻟﺪاﺧﻠﻴﺔ ﻟﺘﺼﻞ إﱃ ) ﺣـﻮاﱄ 80 إﱃ 100 ﻛﻴﻠﻮﻣﱰ ﰲ اﻟﺜﺎﻧﻴـﺔ ( وﻣـﻊ ذﻟـﻚ ﻓـﺈن اﻟﻔﺮق ﰲ اﻟﴪـﻋﺔ ﺑـ ﻫـﺬه اﻷﺟـﺰاء ﻣـﻦ اﻟﺘﺪﻓﻖ اﻟﺨﺎرﺟﻲ و ﻣﻮﺟﺔ اﻟﺼﺪﻣﺔ - أﺻـﻐﺮ . ﺑﻜﺜ ﺧﻠﺺ اﻟﺒﺎﺣﺜﻮن إﱃ أن اﻟﺘﺪﻓﻘ ﺎت ﻣﻦ اﻟﻨﺠﻮم اﻷﺣﺪث ﺳﻨﺎ ﻣﺜﻞ ﺗﻠﻚ ا ﻮﺟﻮدة ﰲ ﻣﺮﻛﺰ HH 211 ﺗﺘﻜﻮن ﰲ ﻣﻌﻈﻤﻬﺎ ﻣـﻦ ﺟﺰﻳﺌـﺎت ﻷن ﴎﻋﺎت ﻣﻮﺟﺔ اﻟﺼﺪﻣﺔ ا ﻨﺨﻔﻀـﺔ ﻧﺴـﺒﻴﺎً ﻟﻴﺴﺖ ﻧﺸﻄﺔ ﺑﻤﺎ ﻳﻜﻔﻲ ﻟﺘﻔﻜﻴﻚ اﻟﺠﺰﻳﺌـﺎت إﱃ ذرات وأﻳﻮﻧﺎت أﺑﺴﻂ . ﻧﻮﻓﻤﺒﺮ - ﺩﻳﺴﻤﺒﺮ 2 0 2 3