Free Astronomy Magazine January-February 2026 ARABIC VERSION

standing the processes of stel- lar and planetary formation andevolution.However,be- causeMdwarfsareintrinsically faint, detailed observations have historically been limited, and early surveys suggested that more than 70% of them weresinglestars.Recentad- vancesinobservationaltech- niques have revealed this observation to be incomplete: thefrequencyoflow-massstel- lar and substellar companions, such as brown dwarfs, may have been significantly under- estimated. Understanding how oftensuchcompanionsoccur— andtheirmassdistribution—isessen- tialfordistinguishingthesimilarities anddifferencesbetweenplanetfor- mation and star formation. Thekeytothisdiscoverywasathree- prongedobservationalapproachin- cluding Keck Observatory, Subaru TelescopeandtheGaiaMission:(1) radial velocity measurements from long-term infrared spectroscopic monitoring with Subaru’s InfraRed Doppler(IRD)trackedthesubtle wobble of the host star, caused by their mutual gravitational pull; (2) high-resolutionnear-infraredimag- ingfromKeckObservatory’sstate-of- the-art adaptive optics on itsNear- Infrared camera (NIRC2) en- abled the direct detection of the companion at a very small separa- tion from its host star; and (3) the Gaiamissiontrackedtinychangesin thestar’spositionintheskytofur- therrevealthegravitationalpull intooperation.”    JANUARY-FEBRUARY2026 I nfrared imageofthe browndwarf companion J1446B (marked by the arrow). Thehoststar (J1446) is masked in white during imageprocess- ing.Thewhite baratthe lowerrightcorrespondstoanangulardistanceequiv- alent to 10 astronomical units (roughly the distance between Saturn and the Sun). [Taichi Uyama (Astro- biology Center/CSUN) / W. M. Keck Observatory] ﻣﺠﻠﺔ FreeAstronomy ﺎﻟﻌﺮ ﺔ 6 اﻟﻘﺰﻣﺔ اﻟﺤﻤـﺮاء ﺿـﻌﻴﻔﺔ اﻹﺷـﻌﺎع ﺑﻄﺒﻴﻌﺘﻬﺎ ﻛﺎﻧﺖ اﻷرﺻﺎد اﻟﺘﻔﺼـﻴﻠﻴﺔ ﻟﻬــﺎ ﻣﺤــﺪودة ﺗﺎرﻳﺨﻴــﺎً وأﺷــﺎرت اﻟﺪراﺳﺎت اﻷوﻟﻴﺔ إﱃ أن أﻛﺜﺮ ﻣﻦ 70 % ﻣﻨﻬﺎ ﻧﺠﻮم ﻣﻔﺮدة . ﻟﻜ ـﻦ اﻟﺘﻘ ـﺪم ا ﻟﺤ ـﺪﻳﺚ ﰲ ﺗﻘﻨﻴ ـﺎت اﻟﺮﺻﺪ ﻛﺸﻒ أن ﻫﺬ ا اﻟﺮ ﻛﺎن ﺻﺪ ﻏ : ﻣﻜﺘﻤﻞ ﻓﻘﺪ ﺗﻢ ﺗﻘﺪﻳﺮ ﺗﻜﺮار اﻟﺮﻓـ ﺎق اﻟﻨﺠﻤﻴ ي اﻟﻜﺘﻞ و ذ ا ﻨﺨﻔﻀﺔ ﻣﺜـﻞ اﻷﻗﺰام اﻟﺒﻨﻴﺔ ﺑﺄﻗﻞ ﻣﻦ اﻟﻮاﻗﻊ ﺑﺸﻜﻞ إن . ﻛﺒ ﻓﻬﻢ ﻣﺪى ﺗﻜﺮار وﺟﻮد ﻣﺜـﻞ اﻷﺟﺮام ﻫﺬه ا ﺮاﻓﻘﺔ وﺗﻮزﻳﻊ ﻛﺘﻠﻬـﺎ أﻣﺮ أﺳﺎﳼ ﻟﻠﺘﻤﻴﻴﺰ ﺑ أوﺟﻪ اﻟﺘﺸﺎﺑﻪ واﻻﺧ ـﺘﻼف ﺑ ـ ﺗﺸ ـﻜﻞ اﻟﻜﻮاﻛ ـﺐ وﺗﺸﻜﻞ اﻟﻨﺠﻮم . ﻟﻘﺪ ﻛﺎن ا ﻔﺘـﺎح ﰲ ﻫﺬا اﻻﻛﺘﺸﺎف ﻫﻮ ﻧﻬﺞ رﺻﺪي ﺛﻼﺛﻲ ا ﺤﺎور ﺷﻤﻞ ﻣﺮﺻﺪ ﻛﻴﻚ و ﺗﻠﺴﻜﻮب ﺳﻮﺑﺎرو وﻣﻬﻤﺔ : ﺎﻳﺎﻏ 1 . ﻗﻴﺎﺳﺎت اﻟـ ـ ﴪﻋﺔ اﻟﺸـﻌﺎﻋﻴﺔ ﻣـﻦ ا ﺮاﻗﺒﺔ اﻟﻄﻴﻔﻴـﺔ ﺑﺎﻷﺷـﻌﺔ ﺗﺤـﺖ اﻟﺤﻤـﺮاء ﻃﻮﻳﻠﺔ ا ﺪى ﺑﺎﺳﺘﺨﺪام ﺟﻬﺎز دوﺑﻠﺮ ﺑﺎﻷﺷﻌﺔ ﺗﺤﺖ اﻟﺤﻤﺮاء (IRD) ﻋﲆ ﺗﻠﺴﻜﻮب ﺳﻮ ﺑﺎرو واﻟﺬي ﺗﺘﺒﻊ اﻻﻫﺘﺰاز اﻟﻄﻔﻴﻒ ﻟﻠﻨﺠﻢ ا ﻀـﻴﻒ اﻟﻨﺎﺗﺞ ﻋﻦ اﻟﺠﺬب ا ﺘﺒﺎدل ﺑﻴﻨﻪ وﺑ اﻟﺠﺴـﻢ اﻟﺮﻓﻴﻖ .2 . اﻟﺘﺼﻮﻳﺮ ﻋﺎﱄ اﻟﺪﻗﺔ ﺑﺎﻷﺷﻌﺔ ﺗﺤﺖ اﻟﺤﻤﺮاء اﻟﻘﺮﻳﺒﺔ ﺑﺎﺳﺘﺨﺪام ﻧﻈﺎم اﻟ ـ ﺒﴫﻳﺎت ـــــــــــــــــــــــــــــــــــــ اﻟﺘﻜﻴﻔﻴﺔ ا ﺘﻄﻮر ﺮﺻﺪ ﻛﻴـﻚ ﻋـﲆ اﻟﻜـﺎﻣ ا اﻟﻘﺮﻳﺒﺔ ﻣﻦ اﻻﺷﻌﺔ ﺗﺤﺖ اﻟﺤﻤـﺮاء (NIRC2) ﻣﻤﺎ أﺗﺎح اﻟﻜﺸﻒ ا ﺒﺎﴍ اﻟﺠﺮم ﻋﻦ ا ﺮاﻓـﻖ ﻋﲆ ﻣﺴﺎﻓﺔ ﺻﻐ ة ﺟﺪًا ﻣﻦ اﻟﻨﺠﻢ ا ﻀـﻴﻒ . 3 . ﻣﻬﻤﺔ ﺟﺎﻳﺎ اﻟﺘﻲ ﺗﺘﺒﻌﺖ اﻟﺘﻐ ات اﻟﻄﻔﻴﻔﺔ ﰲ ﻣﻮﻗﻊ اﻟﻨﺠﻢ ﰲ اﻟﺴﻤﺎء ﻟﻜﺸﻒ ا ﺰﻳـﺪ ﻋـﻦ ﺗﺄﺛ اﻟﺠﺬب اﻟﻨﺎﺗﺞ ﻋﻦ اﻟﺠﺮم ا ﺮاﻓـﻖ . ﻣـﻦ ﺧﻼل دﻣﺞ ﻫﺬه اﻟﺒﻴﺎﻧﺎت وﺗﻄﺒﻴﻖ ﻗﻮاﻧ ﻛﺒﻠﺮ ﺗﻤﻜﻦ اﻟﻔﺮﻳﻖ ﻣﻦ ﺗﺤﺪﻳﺪ اﻟﻜﺘﻠﺔ اﻟﺪﻳﻨﺎﻣﻴﻜﻴـﺔ وﺧﺼﺎﺋﺺ ا ـﺪار ﻟﻠﺠـﺮم ا ﺮاﻓـﻖ J1446B ـــــــــــــــــــــــــــــــــــــ ﺑﺪﻗﺔ ﻏـ ﻣﺴـﺒﻮ . ﻗﺔ ﻗـﺎل ﺗﺸـﺎرﻟﺰ ﺑﻴﺸﻤﺎن ا ﺪﻳﺮ اﻟﺘﻨﻔﻴﺬي ﻌﻬﺪ ﻧﺎﺳـﺎ ﻟﻌﻠﻮم اﻟﻜﻮاﻛﺐ اﻟﺨﺎرﺟﻴﺔ (NExScI) ﰲ ﻛﺎﻟﺘ ﻴﻚ وا ﺆﻟﻒ ا ﺸﺎرك ﰲ اﻟﺪراﺳﺔ : ﺖﻛﺎﻧ" ا ﺴﺎﻫﻤﺔ اﻟﻬﺎﻣﺔ ﺮﺻﺪ ﻛﻴـﻚ ﻫﻲ اﻟﺤﺼﻮل ﻋﲆ ﺻﻮر ﻣﺒﺎﴍة ﻟﻬﺬا اﻟﻘﺰم اﻟﺒﻨﻲ اﻟﺮﻓﻴﻖ ﻣﻤـﺎ ﻣﻜـ ﻦ ﻣـﻦ ﺗﺤﺪﻳﺪ ﻣﺪاره وﺧﺼﺎﺋﺼﻪ اﻟﻔﻴﺰﻳﺎﺋﻴـﺔ ﻣ ﺜﻞ اﻟﻜﺘﻠﺔ ودرﺟﺔ اﻟﺤﺮارة ". ﻳﻮﻓﺮ اﻛﺘﺸﺎف J1446B ﺎُ ﻣﻬﻤ اً ﻣﻌﻴﺎر ﻻﺧﺘﺒﺎر ﺳﻴﻨﺎرﻳﻮﻫﺎت ﺗﻜﻮّن اﻷﻗـﺰام اﻟﺒﻨﻴﺔ وﻧﻤﺎذج اﻟﻐﻼف اﻟﺠﻮي اﻟﺨﺎﺻﺔ . ﺑﻬﺎ إن اﻟﺠﻤﻊ ﺑ إﺻﺪارات ﺑﻴﺎﻧـﺎت ﺟﺎﻳﺎ ا ﺴﺘﻘﺒﻠﻴﺔ واﻟﺒﻴﺎﻧـﺎت اﻟﻄﻴﻔﻴـﺔ ا ﺘﻘﺪﻣﺔ اﻟﻨﺎﺗﺠﺔ ﻋﻦ اﻷرﺻﺎد اﻟﻼﺣﻘﺔ ﺑﺎﺳﺘﺨﺪ ام أﺟﻬﺰة ﺟﺪﻳﺪة ﻣﺜﻞ ﺟﻬﺎز ﻫﺎﻳﺴﺒﻚ ) ﻣﻘﻴﺎس ﻃﻴﻔﻲ ﺑﺎﻷﺷﻌﺔ ﺗﺤﺖ اﻟﺤﻤﺮاء ﻋﺎﱄ اﻟﺪﻗﺔ ﻟﺘﻮﺻﻴﻒ اﻟﻜﻮاﻛﺐ اﻟﺨﺎرﺟﻴﺔ ( ﰲ ﻣﺮﺻﺪ ﻛﻴﻚ ﻗﺪ ﻳ ﻤﻜﻦ اﻟﺒـﺎﺣﺜ ﻣـﻦ رﺳـﻢ أﻧﻤـﺎط اﻟﻄﻘﺲ ﻣﺎ ﻳﻤﺜﻞ ﺧﻄـﻮة ﻣﻬﻤـﺔ ﻧﺤـﻮ ﻓﻬـﻢ ﺸﻜﻞ ﺗ وﺗﻄﻮر اﻟﻜﻮاﻛﺐ ورﺑﻤـﺎ ﻳﻘﻮدﻧـﺎ ذﻟـﻚ ﺎً ﻳﻮﻣ إﱃ اﻛﺘﺸﺎف ﻛﻮﻛـﺐ ﻣﺸـﺎﺑﻪ ﻟﻜﻮﻛﺒﻨـﺎ . وأﺿــﺎف ﺗﺸــﺎ رﻟﺰ ﺑﻴﺸــﻤﺎن :” ا ــﺬﻫﻞ أن ﺻﻮرﺗ ﻣﻦ ﻛﻴﻚ أﻇﻬ ﺮﺗـﺎ ﺗﻐـ اً ﰲ ﺳـﻄﻮع اﻟﻘﺰم اﻟﺒﻨـﻲ ﻣﻤـﺎ ﻳﺸـ إﱃ وﺟـﻮد ﺳـﺤﺐ ﺳﺤﺐ وأﻧﻤﺎط ﺟﻮﻳﺔ ! ﻫـﺬا اﻟـﻨﻬﺞ ا ﺸـﱰك وأﻧﻤﺎط ﺟﻮﻳـﺔ ! ﻫـﺬا اﻟـﻨﻬﺞ ا ﺸﱰك ﺳﻴﺼﺒﺢ أﻗﻮى وأﻛﺜﺮ ﻗﺪرة ﻣﻊ ﻣﺮور اﻟﻮﻗﺖ، ﻟﻴﺼﻞ ﺣﺘــﻰ إﱃ ﻋــﺎﻟﻢ اﻟﻜﻮاﻛــﺐ اﻟﻐﺎ زﻳﺔ اﻟﻌﻤﻼﻗﺔ ﻣﺜﻞ ﻛﻮﻛﺐ ا ﺸـﱰي ﻣـﻊ ﺑـﺪء ﺗﺸـﻐﻴﻞ أﺟﻬﺰة ﺟﺪﻳﺪة ﰲ ﻣﺮﺻﺪ ﻛﻴﻚ . ﻣ ــﻊ اﺳــﺘﻤﺮار ﺗﺤﺴ ــ اﻟﺘﻘﻨﻴﺎت ﺳﻴﻜﻮن ﺑﺎﻹﻣﻜـﺎن دراﺳــﺔ ﺗﻐــ ات اﻟﻄﻘــﺲ وا ﻨــﺎخ ﰲ اﻷﻗــﺰام اﻟﺒﻨﻴــﺔ واﻟﻜ ﻮاﻛﺐ اﻟﺨﺎرﺟﻴﺔ ﺑﺸـﻜﻞ أﻛﺜـﺮ ﺗﻔﺼـﻴﻼً ﻣﻤـﺎ ﻳﻔـﺘﺢ ا ﺠﺎل ﻟﻔﻬﻢ أﻋﻤـﻖ ﻟﺘﻜـﻮﻳ ﻦ اﻟﻜﻮاﻛـﺐ و ﺗﻄـﻮر اﻷﻧﻈﻤـﺔ اﻟﻨﺠﻤﻴﺔ ﻳﺘﻢ ورﺑﻤﺎ اﻛﺘﺸـﺎف ﺑﻴﺌــﺎت ﺻــﺎﻟﺤﺔ ﻟﻠﺤﻴــﺎة ﰲ ا ﺴﺘﻘﺒﻞ اﻟﻘﺮﻳﺐ . ﺻـــــﻮرة ﺎﻷﺷـــــﻌﺔ ﺗﺤـﺖ اﻟـ ـ ﻤﺮاء ﻟﻠﻘـﺰم اﻟﻤﺮاﻓــــــــــــــــــﻖ ــــــــــــــــــ اﻟ J1446B ) ﻣﻮﺳـــــﻮم ﺎﻟﺴــــــــــﻬﻢ .( اﻟــــــــــﻨ ﻢ اﻟﻤﻀــــــــــــــــــــــــ ﻒ J1446 ـــــــــــــــﺎﻟﻠﻮن ﻣﻐﻄّـــــــــــــــﻰ اﻷﺑــــــــــــــــــــــــ ﺾ أﺛﻨــــــــــــــــــــــــﺎء ـ ﻣﻌﺎﻟـــــــــ ﺠﺔ اﻟﺼـــــــــﻮرة . اﻟﺸـــــــــــــﺮﻂ اﻷﺑـــــــــــــ ﺾ ﻓـــــــﻲ أﺳـــــــﻔﻞ ﻤـــــــ اﻟﺼـــــــــــــــــــــﻮرة ﻤﺜـــــــــــــــــــــﻞ ّـــــــــــــــــــﺔ ﻣﺴــــــــــــــــــﺎﻓﺔ زاو ﺗ ﻌــــــــــﺎدل ١٠ وﺣــــــــــﺪات ًـــــــــــــــــــــــﺎ ــــــــــــــــــــــﺔ ﺗﻘﺮ ﻓﻠﻜ ) ﺣـــــﻮاﻟﻲ اﻟﻤﺴـــــﺎﻓﺔ ـــﺎدل 10 ـــ ـــﺔ ﺗﻘﺮ ﺣـــﺪات ﻓﻠﻜ ) ﺎً ﺣـــﻮاﻟﻲ اﻟﻤﺴـــﺎﻓﺔ ﺑـــ ﻮﻛـــﺐ زﺣـــﻞ واﻟﺸـــــﻤﺲ ( و ﻈﻬـــــﺮاﻟﺘﻔﺎﺻـــــﻴﻞ اﻟﺪﻗ ﻘــــــﺔ ﻟﻠﻐـــــﻼف اﻟــــــﺠﻮيوﻇــــــﻮاﻫﺮ اﻟﻤﺮاﻓﻖ ﺸ ﻞ واﺿﺢ ﺗﻤﺎﻣﺎً اﻟﺴﻄﻮع ﺘﻐ ة ﻟﻠﻘﺰم اﻟ . [Taichi Uyama (Astrobiology Center/CSUN) / W. M. Keck Observatory] - ﻳﻨﺎﻳﺮ ﻓﺒﺮﺍﻳﺮ 2 0 2 6 ﻧﻤﺬﺟــﺔ ﻣــﺪار J1446B :- ـ اﻟــ ﺠﺎﻧﺐ اﻷ ﺴـــﺮ : اﻟﻤــﺪار اﻟﻤﺘﻮﻗــﻊ اﻟﻤﺴـــﺘﻨﺘﺞ ﻣــﻦ اﻟﺘﺼــﻮﻳﺮ اﻟﻤ ﺎﺷــﺮﻟﻤﺮ . إم. ﺻـــﺪ د ﻠﻴــﻮ ــﻚ ) ﻛ اﻟﻨﻘﻄـــﺔ اﻟﺰرﻗﺎء ﻓﻲ اﻷﻋﻠﻰﺟﻬﺔ اﻟ ﻤ ( واﻟﺘﺴﺎرع ﻓﻲﺣﺮﻛﺔ اﻟﻨ ﻢ اﻟﻤﻀـ ﻒ اﻟﻤﻘـﺎس ﺑﻮاﺳـﻄﺔ ـﺎ ﻏ ) ﺎ اﻟﺴـﻬﻢ اﻷ ﻤـﺮ .( اﻟﻤﺤـﺎورﺗﻤﺜـﻞ اﻟﺼﻌﻮد اﻟﻤﺴﺘﻘ ﻢ واﻟﻤﻴﻞ ﺎﻟﺜﻮاﻧﻲ اﻟﻘﻮﺳ ﺔ . اﻷﺳـﻮد اﻟﻤـﺪار اﻷﻛـ اﺣﺘﻤـﺎﻻً ﻤﺜﻞ اﻟﻤﻨﺤ ـﺎت ﺑ ﻨﻤـﺎ ﺗﺸـ اﻟﻤﻨﺤﻨ اﻟﻤﻠﻮﻧـﺔ إﻟـﻰ ﻣﺪارا ت ﻣﺤﺘﻤﻠﺔ أﺧـﺮى ـﺚ ﺣ اﻟﻠـﻮن ﻌﻜـﺲ اﻟﻜﺘﻠـﺔ اﻟﻤﻘـﺪرة ﻟــ J1446B ) ـﺎس اﻷﻟـﻮان ﻋﻠـﻰ اﻟ ﻤـ ﻣﻘ ـ اﻟـ –(. ﺠﺎﻧﺐ اﻷ ﻤـﻦ : ﺗﻐـ ات اﻟﺴـﺮ ﻋﺔ اﻟﺸــﻌﺎﻋ ﺔ ﻟﻠــﻨ ﻢ اﻟﻤﻀـ ﻒ اﻟﻤﻘﺎﺳــ ﮫ ﺑﻮاﺳــﻄﺔ IRD ) اﻟﻨﻘـﺎط اﻟــ ـ ( ﻤﺮاء إﻟـﻰﺟﺎﻧـﺐﺣﻠــﻮل ـﺎة ﻣﻠﻮﻧــﺔ ﺣﺴــﺐ ﻣﺪار ــﺔ ﻣﺤﺎ ﻛﺘﻠﺔ ا ﻟـﺠﺮم اﻟﻤﺮاﻓﻖ . ﻈﻬﺮ اﻟﻠﻮﺣﺔ اﻟﺴﻔﻠ ﺔ اﻟﺒ ﻮاﻗﻲ اﻟﻨﺎﺗﺠﺔ ﻋﻦ اﻟﻤﻼﺋﻤﺔ . [Qier An (UCSB) / Uyama et al. (2025)]