Введение
Многозвездная система в созвездии Лебедя.
Starbox observe 2s
| epoch = J2000.0
| constell = Cygnus
| component1 = 16 Cygni A
| ra1 =
| metal fe = 0.101 ± 0.008
| age gyr = 7.07 The orbital elements of the A–C binary are currently unknown. At a distance of 860 AU from A is a third component designated 16 Cygni B. The orbit of B relative to the A–C pair was determined in 1999 and not updated since (as of June 2007): plausible orbits range in period from 18,200 to 1.3 million years, with a semimajor axis ranging from 877 to 15,180 AU. In addition B orbits between 100 and 160 degrees inclination, that is against the A–C pole such that 90 degrees would be ecliptical. Both 16 Cygni A and 16 Cygni B are yellow dwarf stars similar to the Sun. Their spectral types have been given as G1.5V and G3V, with A being a little hotter than the Sun, and B somewhat cooler. The system was within the field of view of the original mission of the Kepler spacecraft, which collected extremely precise photometric data of the stars. From these measurements, asteroseismology models have calculated precise masses of 1.08 and 1.04 times the solar mass for 16 Cygni A and 16 Cygni B respectively, and independent ages of around 7 billion years for each star. The angular diameters together with the asteroseismology models were used to calculate radii of 1.229 and 1.116 times the solar radius for components A and B respectively. Another chemical peculiarity between the stars is in their lithium abundance. Measurements of the lithium abundance in the system show a 4 times higher abundance in component A than in 16 Cygni B. Compared to the Sun, 16 Cygni A has 1.66 as much lithium, while 16 Cygni B has only 0.35. It has been hypothesized that the accretion of about 1 Earth mass of metals by 16 Cygni B soon after the system's formation may have destroyed the lithium in the star's atmosphere.
Наблюдения Starbox: 2с
| эпоха = J2000.0
| созвездие = Лебедь
| компонент1 = 16 Лебедя A
| ra1 =
| металл Fe = 0.101 ± 0.008
| возраст gyr = 7.07
Starbox observe 2s
| epoch = J2000.0
| constell = Cygnus
| component1 = 16 Cygni A
| ra1 =
| metal fe = 0.101 ± 0.008
| age gyr = 7.07 The orbital elements of the A–C binary are currently unknown. At a distance of 860 AU from A is a third component designated 16 Cygni B. The orbit of B relative to the A–C pair was determined in 1999 and not updated since (as of June 2007): plausible orbits range in period from 18,200 to 1.3 million years, with a semimajor axis ranging from 877 to 15,180 AU. In addition B orbits between 100 and 160 degrees inclination, that is against the A–C pole such that 90 degrees would be ecliptical. Both 16 Cygni A and 16 Cygni B are yellow dwarf stars similar to the Sun. Their spectral types have been given as G1.5V and G3V, with A being a little hotter than the Sun, and B somewhat cooler. The system was within the field of view of the original mission of the Kepler spacecraft, which collected extremely precise photometric data of the stars. From these measurements, asteroseismology models have calculated precise masses of 1.08 and 1.04 times the solar mass for 16 Cygni A and 16 Cygni B respectively, and independent ages of around 7 billion years for each star. The angular diameters together with the asteroseismology models were used to calculate radii of 1.229 and 1.116 times the solar radius for components A and B respectively. Another chemical peculiarity between the stars is in their lithium abundance. Measurements of the lithium abundance in the system show a 4 times higher abundance in component A than in 16 Cygni B. Compared to the Sun, 16 Cygni A has 1.66 as much lithium, while 16 Cygni B has only 0.35. It has been hypothesized that the accretion of about 1 Earth mass of metals by 16 Cygni B soon after the system's formation may have destroyed the lithium in the star's atmosphere.
Орбитальные элементы двойной системы A–C в настоящее время неизвестны. На расстоянии 860 а.е. от A находится третий компонент, обозначенный как 16 Лебедя B. Орбита B относительно пары A–C была определена в 1999 году и с тех пор не обновлялась (по состоянию на июнь 2007 года): вероятные орбиты имеют период от 18 200 до 1,3 миллиона лет, с большой полуосью от 877 до 15 180 а.е. Кроме того, орбита B имеет наклон от 100 до 160 градусов, то есть направлена против полюса A–C, так что наклон в 90 градусов соответствовал бы эклиптике. И 16 Лебедя A, и 16 Лебедя B — желтые карлики, подобные Солнцу. Их спектральные типы определены как G1.5V и G3V, при этом A немного горячее Солнца, а B несколько холоднее. Система находилась в поле зрения первоначальной миссии космического аппарата «Кеплер», который собрал чрезвычайно точные фотометрические данные о звездах. На основе этих измерений модели астеросейсмологии рассчитали точные массы в 1,08 и 1,04 раза больше массы Солнца для 16 Лебедя A и 16 Лебедя B соответственно, а также независимые оценки возраста около 7 миллиардов лет для каждой звезды. Угловые диаметры, совместно с моделями астеросейсмологии, были использованы для расчета радиусов в 1,229 и 1,116 раза больше радиуса Солнца для компонентов A и B соответственно. Другая химическая особенность звезд заключается в их содержании лития. Измерения содержания лития в системе показывают, что в компоненте A его в 4 раза больше, чем в 16 Лебедя B. По сравнению с Солнцем, 16 Лебедя A содержит 1,66 массы лития, в то время как 16 Лебедя B — всего 0,35. Предполагается, что аккреция 16 Лебедем B около 1 массы Земли металлов вскоре после формирования системы могла привести к разрушению лития в атмосфере звезды.
Starbox observe 2s
| epoch = J2000.0
| constell = Cygnus
| component1 = 16 Cygni A
| ra1 =
| metal fe = 0.101 ± 0.008
| age gyr = 7.07 The orbital elements of the A–C binary are currently unknown. At a distance of 860 AU from A is a third component designated 16 Cygni B. The orbit of B relative to the A–C pair was determined in 1999 and not updated since (as of June 2007): plausible orbits range in period from 18,200 to 1.3 million years, with a semimajor axis ranging from 877 to 15,180 AU. In addition B orbits between 100 and 160 degrees inclination, that is against the A–C pole such that 90 degrees would be ecliptical. Both 16 Cygni A and 16 Cygni B are yellow dwarf stars similar to the Sun. Their spectral types have been given as G1.5V and G3V, with A being a little hotter than the Sun, and B somewhat cooler. The system was within the field of view of the original mission of the Kepler spacecraft, which collected extremely precise photometric data of the stars. From these measurements, asteroseismology models have calculated precise masses of 1.08 and 1.04 times the solar mass for 16 Cygni A and 16 Cygni B respectively, and independent ages of around 7 billion years for each star. The angular diameters together with the asteroseismology models were used to calculate radii of 1.229 and 1.116 times the solar radius for components A and B respectively. Another chemical peculiarity between the stars is in their lithium abundance. Measurements of the lithium abundance in the system show a 4 times higher abundance in component A than in 16 Cygni B. Compared to the Sun, 16 Cygni A has 1.66 as much lithium, while 16 Cygni B has only 0.35. It has been hypothesized that the accretion of about 1 Earth mass of metals by 16 Cygni B soon after the system's formation may have destroyed the lithium in the star's atmosphere.
Планетарная система
В 1996 году было объявлено об обнаружении экзопланеты на эксцентрической орбите вокруг звезды 16 Cygni B. Открытие, выполненное методом радиальных скоростей, стало результатом независимых наблюдений, проведенных в обсерваториях Макдональда и Лика. Как и большинство экзопланет, обнаруживаемых с Земли, существование 16 Cygni Bb было выведено на основе измерений радиальной скорости ее звезды. В то время это позволило определить лишь нижний предел массы: в данном случае, около 1,68 массы Юпитера. В 2012 году два астронома, Е. Плавалова и Н. А. Соловая, показали, что для обеспечения стабильности орбиты требуется масса около 2,38 массы Юпитера, при этом орбита должна быть наклонена либо на 45°, либо на 135°.