Free Astronomy Magazine July-August 2026 ARABIC VERSION

awaytomuchhighermassesthan29 Cygni b. This is the lowest mass you could plausibly get. But at the same time,it’saboutthehighestmassyou could get from accretion,” said lead author William Balmer of the Johns Hopkins University and the Space Telescope Science Institute, both in Baltimore. Balmer’s observing program used Webb’s NIRCam (Near-Infrared Cam- era) in its coronagraphic mode to di- rectlyimage29Cygnib.Thisplanet wasthefirstoffourobjectstarget- edbytheprogram,allofwhichare known to weigh between 1 and 15 times as much as Jupiter. The team also required their targets to orbit within about 9 billion miles (15 bil- lion kilometers) of their stars. Theplanetswereallyoungandstill hotfromtheirformation,rangingin temperature from about 1,000 to 1,900 degrees Fahrenheit (530 to 1,000 degrees Celsius). This would ensuretheiratmosphericchemistry was similar to the planets of HR 8799,whosesystemBalmerstudied previously.Bychoosingappropriate filters,theteamwasabletolook for signsoflightbeingabsorbedbycarbondi oxide(CO 2 )andcarbon monoxide (CO), which allowed them to determine the amount of thoseheavierchemicalelements,whic has- tronomers collectively call metals. They found strong evidence that 29 Cygnibisenrichedinmetalsrelative toitshoststar,whichissimilartoour Suninitscomposition.Giventhe planet’s mass, the amount of heavy elements it contains is equivalent to about 150 Earths. This suggests that it accreted large amounts of metal- enriched solids from a protoplane- tary disk. Theteamalsousedaground-based opticaltelescopearraycalledCHARA (CenterforHighAngularResolution Astronomy) to determine if the planet’s orbit is aligned with the spinofthestar.Theyconfirmedthat alignment, which would be ex- pected for an object that formed from a protoplanetary disk. “We were able to update the planet’sorbit,andalsoobservedthe host star to determine its orienta- tionwithrespecttothatorbit,” said Ash Messier, co-author and a gradu- atestudentatJohnsHopkinsUniver- sity. “We showed that the incli- nation of the planet is well-aligned with the spin axis of the star, which is similar to what we see for the planets of our solar system.” “Put together, this evidence strong- ly suggests that 29 Cygni b formed within a protoplanetary diskthrough rapid accretion of metal- rich material, rather than through gasfragmentation,” saidBalmer. “In other words, it formed like a planet and not like a star.” As the team gathers data on the otherthreetargetswithintheirpro- gram,theyplantolookforevidence of compositional differences be- tween the lower-mass and higher- mass planets. This should provide additionalinsightsintotheirforma- tionmechanisms.    JULY-AUGUST2026 ﻣﺠﻠﺔ FreeAstronomy ﺎﻟﻌﺮ ﺔ 14 - ﻳﻮﻟﻴﻮ ﺃﻏﺴﻄﺲ 2 0 2 6 ﰲ ﺑـﺎﻟﺘﻴﻤﻮر :» ﰲ اﻟﻨﻤـﺎذج اﻟﺤﺎﺳـﻮﺑﻴﺔ ﻣـﻦ اﻟﺴﻬﻞ ﺟﺪاً أن ﺗﺆدي ﻋﻤﻠﻴـﺔ اﻟﺘﺠـﺰؤ داﺧـﻞ اﻟﻘﺮص إﱃ ﻛﺘﻞ أﻛﱪ ﺑﻜﺜ ﻣـﻦ 29 Cygni b . ﻫﺬا ﻫﻮ أﻗﻞ ﺣﺪ ﻛ ﺘﲇ ﻳﻤﻜـﻦ اﻟﻮﺻـﻮل إﻟﻴـﻪ ﺑﺸﻜﻞ ﻣ ﻌﻘﻮل ﻟﻜﻨﻪ ﰲ اﻟﻮﻗﺖ ﻧﻔﺴﻪ أﻋﲆ ﺣﺪ ﻳﻤﻜﻦ أن ﻳﻨﺘﺞ ﻋﻦ اﻟﱰاﻛﻢ . « اﺳﺘﺨﺪم ﺑﺮﻧﺎﻣﺞ اﻟﺮﺻـﺪ اﻟﺘـﺎﺑﻊ ﻟِ ﺘﻠﺴـﻜﻮب ﺟﻴﻤﺲ وﻳـﺐ اﻟﻔﻀـﺎﺋﻲ ) ﻛـﺎﻣ ا ﻧ ﻛـﺎم ( ﻟ ﻸﺷﻌﺔ ﺗﺤﺖ اﻟﺤﻤﺮاء اﻟﻘﺮﻳﺒﺔ ﰲ وﺿﻊ ﻣﺤﺪد ﻳﺴﻤﻰ اﻟﻜﻮروﻧﻮﻏﺮاﻓﻴﻚ ﻟﺘﺼﻮﻳﺮ 29 Cygni b . ﻣﺒﺎﴍة وﻛﺎن ﻫﺬا اﻟﻜﻮﻛﺐ أول ﻫـﺪف ﻣـﻦ ﺑـ أرﺑﻌـﺔ أﻫـﺪاف ﰲ اﻟﱪﻧـﺎﻣﺞ، ﺟﻤﻴﻌﻬـﺎ أﺟﺴﺎم ﻣﻌﺮوﻓﺔ ﺑﻜﺘﻠـﺔ ﺗـﱰاوح ﺑـ 1 و 15 ﻣﺮة ﻛﺘﻠﺔ ا ﺸﱰي . ﻛﻤﺎ اﺷـﱰط اﻟﻔﺮﻳـﻖ أن ﻣﺮة ﻛﺘﻠـﺔ ﻛﻮﻛـﺐ ا ﺸـﱰي . ﻛﻤـﺎ اﺷـﱰط اﻟﻔﺮﻳﻖ أن ﺗﺪور ﻫﺬه اﻷﺟـ ﺮا م ﻋـﲆ ﻣﺴـﺎﻓﺔ ﺗﺼﻞ إﱃ ﻧﺤـﻮ 9 ﻣﻠﻴـﺎرات ﻣﻴـﻞ )15 ﻣﻠﻴـﺎر ﻛﻴﻠ ـﻮﻣﱰ ( ﻣــﻦ ﻧﺠﻮﻣﻬ ـﺎ . وﻛﺎﻧ ـﺖ ﺟﻤﻴ ـﻊ اﻟﻜﻮاﻛﺐ ا ﺴﺘﻬﺪﻓﺔ ﻓﺘﻴ ﺔ وﻣﺎ ﺗـﺰال ﺳـﺎﺧﻨﺔ ﻧﺘﻴﺠﺔ ﺗﺸﻜّﻠﻬﺎ وﺗﱰاوح درﺟﺎت ﺣﺮارﺗﻬﺎ ﺑ 1000 و 1900 درﺟــﺔ ﻓﻬﺮﻧﻬﺎﻳــﺖ ) 530 إﱃ 1000 درﺟﺔ ﻣﺌﻮﻳﺔ ( وﻫﺬا ﻳﻀﻤﻦ أن ﻛﻴﻤﻴﺎء اﻟﻐﻼف اﻟﺠﻮي ﻟﺪﻳﻬﺎ ﻣﺸﺎﺑﻬﺔ ﻟﻜﻮاﻛﺐ ﻧﻈـﺎم HR 8799 اﻟﺬي درﺳﻪ ﺑﺎ ﺮ . ﺳﺎﺑﻘﺎً وﺑﺎﺧﺘﻴﺎر ﻣﺮﺷﺤﺎت ﻣﻨﺎﺳﺒﺔ ﺗﻤﻜﻦ اﻟﻔﺮﻳﻖ ﻣﻦ اﻟﺒﺤـﺚ ﻋﻦ ﻋﻼﻣﺎت اﻣﺘﺼﺎص اﻟﻀﻮء ﺑﻮاﺳﻄﺔ ﺛﺎﻧﻲ أﻛﺴﻴﺪ اﻟﻜﺮﺑﻮن وأول أﻛﺴﻴﺪ اﻟﻜﺮﺑـﻮن ﻣﻤـﺎ ﺳﻤﺢ ﺑﺘﺤﺪﻳﺪ ﻛﻤﻴﺔ اﻟﻌﻨﺎﴏ اﻟﺜﻘﻴﻠﺔ، واﻟﺘـﻲ ﻳﻄﻠـﻖ ﻋﻠﻴ ﻬـﺎ اﻟﻔﻠﻜﻴـﻮن اﺳـﻢ » ا ﻌـﺎدن «. ﺳﻤﺢ ﺑﺘﺤﺪﻳﺪ ﻛﻤﻴﺔ اﻟﻌﻨﺎﴏ اﻟﺜﻘﻴﻠـﺔ واﻟﺘـﻲ ﻳﻄﻠـﻖ ﻋﻠﻴﻬـﺎ اﻟﻔﻠﻜﻴـﻮن اﺳـﻢ » ا ﻌـﺎدن « . ووﺟﺪوا دﻟﻴﻼً ﻗﻮﻳﺎً ﻋﲆ أن Cygni b 29 ﻏﻨـﻲ ﺑﺎ ﻌﺎدن ﻣﻘﺎرﻧﺔ ﺑﻨﺠﻤﻪ ا ﻀﻴﻒ، اﻟﺬي ﻳﺸﺒﻪ اﻟﺸﻤﺲ ﰲ ﺗﺮﻛﻴﺒﻪ اﻟﻜﻴﻤﻴـﺎﺋﻲ . وﺑـﺎ ﻟﻨﻈﺮ إﱃ ﻛﺘﻠﺔ اﻟﻜﻮﻛﺐ، ﻓﺈن ﻛﻤﻴـﺔ اﻟﻌﻨـﺎﴏ اﻟﺜﻘﻴﻠـﺔ اﻟﺘﻲ ﻳﺤﺘﻮﻳﻬﺎ ﺗﻌﺎدل ﻧﺤﻮ 150 ﻛﺘﻠﺔ أرﺿـﻴﺔ . وﻳﺸ ذﻟﻚ إﱃ أﻧﻪ ﺗﺮاﻛﻢ ﻋﱪ اﻟﺘﻘﺎط ﻛﻤﻴـﺎت ﻛﺒ ة ﻣﻦ ا ﻮاد اﻟﺼﻠﺒﺔ اﻟﻐﻨﻴﺔ ﺑﺎ ﻌـﺎدن ﻣـﻦ ﻗﺮصﻛﻮﻛﺒﻲ أوﱄ . ﻛﻤﺎ اﺳﺘﺨﺪم اﻟﻔﺮﻳﻖ ﻣﺼـﻔﻮﻓﺔ ﺗﻠﺴـﻜﻮﺑﺎت ﺑﴫﻳﺔ أرﺿﻴﺔ ﺗُﻌﺮف ﺑﺎﺳﻢ ﻣﺼﻔﻮﻓﺔ ﺗﺸﺎرا ) ﻣﺮﻛﺰ ﻋﻠﻢ اﻟﻔﻠﻚ ﻋﺎﱄ اﻟﺪﻗﺔ اﻟﺰاوي ( ﻟﺘﺤﺪﻳﺪ ﻣﺎ إذا ﻛﺎن ﻣـﺪار اﻟﻜﻮﻛـﺐ ﻣﺤﺎذﻳـﺎً ﻟـﺪورا ن اﻟﻨﺠﻢ وﺗﺄﻛﺪوا ﻣﻦ ﻫﺬا اﻟﺘﻮاﻓﻖ و ﻫﻮ ﻣﺎ ﻳُﺘﻮﻗﻊ ﺮا ﰲ اﻷﺟ م اﻟﺘﻲ ﺗﺘﺸﻜ ﻞ داﺧﻞ ﻗﺮص ﻛـﻮﻛﺒﻲ . وﻗﺎل آش ﻣﻴﺴ وﻫﻮ ﻃﺎﻟﺐ دراﺳـﺎت ﻋﻠﻴـﺎ وﻣﺸـﺎرك ﰲ اﻟﺪراﺳـﺔ ﻣـﻦ ﺟﺎﻣﻌـﺔ ﺟـﻮﻧﺰ »: ﻨﺰ ﻫﻮﺑﻜ ﺗﻤﻜﻨﺎ ﻣﻦ ﺗﺤﺪﻳﺚ ﻣـﺪار اﻟﻜﻮﻛـﺐ ﻛﻤﺎ رﺻﺪﻧﺎ اﻟﻨﺠﻢ ا ﻀﻴﻒ ﻟﺘﺤﺪﻳـﺪ اﺗﺠﺎﻫـﻪ ﺑﺎﻟﻨﺴﺒﺔ ﻟﻬﺬا ا ﺪار . وأﻇﻬﺮﻧـﺎ أن ﻣﻴـﻞ ﻣـﺪار اﻟﻜﻮﻛﺐ ﻣﺘﻮاﻓـﻖ ﺑﺸـﻜﻞ ﻛﺒـ ﻣـﻊ ﻣﺤـﻮر دوران اﻟﻨﺠﻢ وﻫﻮ ﻣﺎ ﻳﺸﺒﻪ ﻣﺎ ﻧﺮاه ﰲ ﻛﻮاﻛﺐ ﻧﻈﺎﻣﻨﺎ اﻟﺸﻤﴘ . « وﻳُﻌﺪ ﻫﺬا اﻟﺘﻮاﻓﻖ ا ﺪاري ﻣﻦ ا ﺆﴍات ا ﻬﻤﺔ ﰲ ﻋﻠﻢ اﻟﻜﻮاﻛﺐ، ﻷﻧﻪ ﻳﺤﺘﻔﻆ ﺑﺂﺛﺎر اﻟ ﻈـﺮوف اﻟﺘﻲ ﺳﺎدت أﺛﻨﺎء ﺗﺸـﻜﻞ اﻟﻨﻈـﺎم اﻟﻜـﻮﻛﺒﻲ . ﻓﻌﻨﺪﻣﺎ ﺗﻨﺸﺄ اﻟﻜﻮاﻛﺐ داﺧﻞ ﻗﺮص دوّار ﻣـﻦ اﻟﻐﺎز واﻟﻐﺒﺎر ﺣﻮل اﻟـﻨﺠﻢ، ﻓﺈﻧﻬـﺎ ﺗﻤﻴـﻞ إﱃ ﻣﺸﺎرﻛﺔ اﻻﺗﺠﺎه ﻧﻔﺴﻪ ﺗﻘﺮﻳﺒﺎً ﺑﻴﻨﻤﺎ ﻗﺪ ﺗﺆدي آﻟﻴ ـﺎت اﻟﺘﻜ ـﻮّن اﻷﺧـﺮى إﱃ ﻣ ـﺪارات أﻛﺜ ـﺮ اﺿﻄﺮاﺑﺎً واﺧﺘﻼﻓﺎً ﻣﻤﺎ ﻳـﻮﻓﺮ دﻟـﻴﻼً إﺿـﺎﻓﻴﺎً ﻋﲆ اﻟﺘﺎرﻳﺦ اﻟ ﺪﻳﻨﺎﻣﻴﻜﻲ ا ﺒﻜﺮ ﻟﻬـﺬا اﻟﻨﻈـﺎم اﻟﻜﻮﻛﺒﻲ اﻟﻔﺮﻳﺪ . و أﺿﺎف ﺑﺎ ﺮ :» ﻋﻨﺪ ﺟﻤﻊ ﻫﺬه اﻷدﻟـﺔ ﻓﺈﻧﻬـﺎ ﺗﺸ ﺑﻘﻮة إﱃ أن Cygni b 29 ﺗﺸـﻜّﻞ داﺧـﻞ ﻗﺮص ﻛﻮﻛﺒﻲ أوﱄ ﻋﱪ ﺗـﺮاﻛﻢ ﴎﻳـﻊ ـﺎدة ﻏﻨﻴﺔ ﺑﺎ ﻌـﺎدن، وﻟـﻴﺲ ﻋـﱪ ﺗﺠـﺰؤ ﻏـﺎزي . وﺑﻌﺒﺎرة أﺧﺮى، ﻓﻘﺪ ﺗﺸﻜّﻞ ﻛﻜﻮﻛـﺐ وﻟـﻴﺲ « .ﻢﻛﻨﺠ وﻳﺨﻄﻂ اﻟﻔﺮﻳﻖ ﻣﻊ ﺟﻤﻊ ﻣ ﺰﻳﺪ ﻣﻦ اﻟﺒﻴﺎﻧﺎت ﻋﻦ اﻷﻫ ﺪاف اﻟﺜﻼﺛﺔ اﻷﺧـﺮى ﺿـﻤﻦ اﻟﱪﻧﺎﻣﺞ إﱃ اﻟﺒﺤﺚ ﻋـﻦ اﺧﺘﻼﻓـﺎت ﺗﺮﻛﻴﺒﻴـﺔ ﺑ اﻟﻜﻮاﻛﺐ اﻷﻗﻞ ﻛﺘﻠﺔ واﻷﻋﲆ ﻛﺘﻠﺔ ﻣﻤﺎ ﻗـﺪ ﻳﻮﻓﺮ ﻓﻬﻤﺎً أﻋﻤﻖ ﻵﻟﻴﺎت اﻟﺘﻜﻮّن ا ﺨﺘﻠﻔﺔ . اﺳــﺘﺨﺪم ــﺐ اﻟﻔﻀــﺎﺋﻲ اﻟﺘــﺎﺑﻊ ﻟ ﻋﻠﻤــﺎء اﻟﻔﻠــﻚ ﺗﻠﺴــ ﻮبﺟــ ﻤﺲو ﻮ ﺎﻟــﺔ ﻧﺎﺳــﺎ ﻟﺘﺼــﻮﻳﺮ اﻟ ﻮﻛــﺐ اﻟـــﺨﺎرﺟﻲ Cygni b 29 ﻣ ﺎﺷﺮة واﻟﺬ ﺗ ﻠﻎ ﻛﺘﻠﺘﮫ 15 ﺿﻌﻒوزن ﻮﻛﺐ اﻟﻤﺸ ي . ووﺟﺪوا أدﻟﺔ ﻋﻠﻰوﺟﻮد ﻋﻨﺎﺻـﺮ ﻛ ﻤ ﺎ ﺋ ﺔ ﺛﻘ ﻠﺔ ﻣﺜﻞ اﻟﻜﺮﻮن واﻷﻛﺴﺠ ﻣﻤـﺎ ﺸـ ﻘـﻮة إﻟـﻰ أﻧـﮫ ﺗﺸـ ﻞ ﻮﻛـﺐ ﻋـﻦ ﻃﺮ ـﻖ اﻟـ ا ﻢ داﺧـﻞ أوﻟــــﻲ،وﻟ ﺲﻛــــﻨ ﻢ ﻋــــﻦ ﻃﺮ ــــﻖ اﻟﺘﻔﺘــــﺖ ــــﻮﻛ ﻗــــﺮص . ــــﺔ ــــﺎﻣ ا اﻷﺷــــﻌﺔ ﺗﺤــــﺖ ا ﻤــــﺮاء اﻟﻘﺮ اﺳــــﺘﺨﺪﻣﺖ ـــﺎم ) ﻧ ( ــــﺚ ُﺴــــﺘﺨﺪم ـــﺐﺣ اﻟﺘﺎ ﻌــــﺔ ﻟﺘﻠﺴــــ ﻮب و ) ﺣـــﺎﺟﺰ ـــﺎﻟﻤﺮ ﻊ اﻷزرق ــــﮫ ﻣﺸــــﺎر إﻟ ـﻟــــ ( ﺤﺠﺐﺿــــﻮء اﻟــــﻨ ﻢ اﻟﻤﻀ ﻒ ) اﻟﻤﺴﻤﻰ A واﻟﻤُﻤ ﺑﺮﻣﺰ ﻧ ﻤﺔ ( ﻹﻇﻬﺎراﻟ ﻮﻛﺐ . ﺗ ﻤﻊ ﻫﺬﻩ اﻟﺼﻮ رة اﻟﻀﻮء ﻣﻦ ﺛﻼﺛﺔ ﻣﺮﺷﺤﺎت ﺑ 4 و 5 . ﻣ ﻜﺮون ﻳ ﻮن اﻟ ﻮﻛﺐ أﻛ ﺳﻄﻮﻋﺎً ﻓﻲ اﻟﻤﺮﺷﺢ اﻷزرق ﺛﻢ اﻷﺧﻀﺮﺛﻢ اﻷ ﻤﺮﻟﺬا ﻈﻬﺮ ﻛﻨﻘﻄﺔ ـــﺔ اﻟﻤﻠﻮﻧـــﺔ ﺑ ﻀـــﺎء ﻣﺎﺋﻠـــﺔ ﻟﻠﺼـــﻔﺮة ﻓـــﻲ اﻟﺼـــﻮرة اﻟﻤﺮﻛ . ﻟـــﻮ ﻟـــﻢ ﻜـــﻦ ﺛـــﺎﻧﻲ أﻛﺴـــ ﺪ اﻟﻜﺮـــﻮن ﻣﻮﺟـــﻮدًا، ﻟﻈﻬـــﺮ اﻟ ﻮﻛﺐ أﻛ ا ﻤﺮاراً ﺸـ ﻞ ﻣﻠﺤـﻮظ . ﻓـﻲﻫـﺬﻩ اﻟﺼـﻮرة ﻨﺴـﺐ اﻟﻠـﻮن اﻷزرق إﻟـﻰﺿـﻮء ﻃﻮﻟـﮫ اﻟﻤـﻮﺟﻲ 4.1 ﻣ ﻜﺮون واﻷﺧﻀﺮ إﻟﻰﺿﻮء ﻃﻮﻟﮫ اﻟﻤﻮﺟﻲ 4.3 ﻣ ﻜﺮون، واﻷ ﻤﺮإﻟﻰﺿﻮء ﻃﻮﻟﮫ اﻟﻤﻮﺟﻲ 4.6 . ﻣ ﻜﺮون [NASA, ESA, CSA, William Balmer (JHU, STScI), Laurent Pueyo (STScI); Image Processing: Alyssa Pagan (STScI)]