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T矮星

维基百科，自由的百科全书

T矮星或甲烷棕矮星是光谱类型为“T”的天体[1]，这些天体可能是棕矮星[2] 或年轻的自由漂流行星质量天体[3]。一颗直接成像的年轻系外行星也可能是T矮星[4]。T矮星比L矮星冷[1]，但是比Y矮星温暖[5]。

原型：格利泽229B

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主条目：格利泽229
哈伯的格利泽229B的影像。

第一颗被发现的T矮星是1995年发现的格利泽229B[6]。该天体的温度低于1000K，光谱中显示甲烷（CH4）、水蒸气（H2O）和一氧化碳（CO）。 在高层大气中，CO转化为CH4和H2O，而在较热的低层大气中则相反[7][8][9]。它还显示出铯（Cs）的吸收，但缺少M-矮星（一氢化钙（英语：Calcium monohydride）、FeH，TiO和VO中常见的吸收特征[10]。氨（NH3）被纳入光谱分析[11]。钠（Na）和钾（K）也在这颗T矮星中被检测到[12]。后来的研究发现，格利泽229B的动态质量为70±5MJ，远高于冷却模型所建议的质量[2]。光谱类型有些模糊。这是因为它在1.3和1.6μm处显示出强烈的CH4吸收，表明为T7型，但在1.1、1.4、1.9和2.2μm处表现出较弱的CH4和H2O特征，表明为T5-T6型[13]。人们还怀疑格利泽229B是一个双星，这可以解释它的高质量和不寻常的光谱[14]。2024年，甚大望远镜上的仪器证实了这种双星性，该仪器解析了这对双星，并将它们的轨道限制在约16个地月距离的紧密半长轴上，轨道周期约为12.1天。格利泽229Ba的质量约为38MJ，格利泽229Bb的质量约34MJ[15]。

T型光谱

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中晚期T矮星的光谱，显示甲烷、水蒸气、CIA氢和钾的吸收。

光谱类型“T”于1999年首次提出，格利泽229B是当时唯一的代表[1]。接下来是格利泽570D的发现[16]，SDSS 1624+00（第一颗场T矮星）[17]和SDSS 1346-00（第二颗场T矮星）[18]。然而，这些是中晚期的T矮星，第一批早期的T矮星（SDSS 0837、SDSS 1254和SDSS 1021）是在2000年史隆数位巡天的数据中发现的。这些天体显示出比以前发现的T矮星更弱的CH4吸收[19]。CH4首先出现在L8矮星的K波段中，而L矮星和T矮星的区别在于CH4出现在T矮星的H波段。从T0到T8，T矮星对H2O和CH4的吸收逐渐增加。中性Na和K特征在L-和T-矮星中变宽，随着光谱类型的增加，L/T-矮星的Na特征深度也增加[20]。 最冷的T矮星之一是由UKIDSS发现的，名为UGPS 0722-05[21][22]。研究人员使用WISE发现了其他晚期T矮星和新发现的Y矮星天体。在UGPS 0722-05的说明下，T矮星和Y矮星之间的跃迁被定义为T9的标准和WISE 1738+2732作为Y0的标准。晚期T矮星和早期Y矮星表现出深H2O和CH4吸收特征，T矮星和Y矮星之间的跃迁发生在500 K附近[5][23]。另一颗重要的T矮星是卢曼16B，它是距离我们最近的T矮星。它的光谱类型为T0.5，接近L/T跃迁。它在光谱中显示出FeH的痕迹，FeH在晚期L矮星中减弱，但在早期到中期T矮星中由于云层的干扰而增强[24][25]。使用JWST在近红外和中红外波段对T矮星的观测清楚地表明，由于NH3、CH4、H2O、CO和 CO2，T矮星具有额外的吸收特征[26]。双子星天文台的观测表明，在T6矮星DENIS J081730.0−615520中首次检测到硫化氢（H2S）和分子氢（H2）[27]。

次矮星

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主条目：次矮星

已知具有T光谱型的次矮星是2MASSI J0937347+293142，这是第一颗T型次矮星。由于2.1μm峰值的抑制，它显示出蓝色近红外颜色，这可能是由于氢（H2）的碰撞诱导吸收（CIA）增强引起的[28][29]。次矮星的金属丰度较低，起初只知道一个中低金属丰度的小样本。2020年，公民科学项目“后院世界”发现了首批光谱类型为T的极端次矮星，分别命名为“WISEA 0414−5854”和“WISEA 1810−1010”。这些天体具有不寻常的蓝色，表明来自CH4的吸收较低[30]。对WISEA 1810−1010的后续观测表明，它在光学和红外光谱中仅显示出由于H2O和H2引起的吸收。CH4完全缺失，这与T矮星被定义为“甲烷矮星”形成鲜明对比，WISEA 1810−1010被称为“水蒸气矮星”[31]。2024年，布林加斯（英语：Burgasser）等人引入了T次矮星的分类系统，该系统允许分为轻度次矮星（d/sdT）、次矮星（sdT）和极端次矮星（esdT）。低金属性的特征是氢分子的强碰撞诱导吸收（CIA）、模糊的甲烷和水特征以及弱的钾K I吸收。这项工作还确定了三颗棕矮星，它们是恒星流的候选成员。未来与JWST、Euclid、Rubin和Roman的合作将使T次矮星的样本新增到数千个。这项工作还确定了三颗棕矮星，它们是恒星流的候选成员[32]。JWST已经发现了第一颗遥远的T次矮星，例如[UNCOVER-BD-1]][33]。

棕矮星

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主条目：棕矮星

大多数T矮星是棕矮星。棕矮星的质量低于氢燃烧的最小质量（0.075 M☉或78.5 MJ）[34]。 UltracoolSheet 中目前有 920 个红外光谱类型为T的天体[35]。 超冷基本参数表列出了红外光谱类型为T且质量在2到 58 MJ之间的天体[36][37]。其它围绕恒星或白矮星运行的T型棕矮星是已知的，主矮星的年龄可以帮助确定T型矮星的质量[38][39][40]。已知最古老的T矮星之一是Wolf 1130C，它大约有 100亿年的历史。[41]。

行星质量天体和系外行星

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最早被最终确定光谱型为T的年轻孤立行星品质天体之一是SDSS J1110+0116（T5.5），它是1.2亿年老的剑鱼座AB移动星群成员[42]。另一个重要的发现是最近的行星质量天体之一，称为SIMP J013656.5+093347（T2.5，12.7 ±1.0MJ），它是2亿年老的船底座邻近移动星群（英语：Carina-Near moving group）的一部分[3]。这个天体也是变星，周期为2.4小时，可能是由于云层造成的[43]。它还呈现了极光导致的电波发射[44]。其它年轻的T矮星候选者是从其他年轻星协中得知的，与场T矮星相比，这些天体呈现出红色[45]。年轻的直接成像系外行星和行星质量伴星呈现T光谱类型，例如波江座51 b（ T4.5-T6）[4]。

云和可变性

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早期的云模型（SIMP J0136+09，2MASS J2139+02）和晚期的T矮星（2MASS J0050–3322）。

两个变化最大的棕矮星是T矮星卢曼16B，其变化高达20%[46]和2MASS J2139+02，其变化幅度高达26%[47]。T矮星，尤其是年轻的早期型T矮星通常是变星。这种变化与云的存在有关，但也提出了其它解释，例如热点和极光[48]。这些早期的T矮星被认为有一个铁云层和一个斑驳的硅酸盐云层。硅酸盐云被认为在 L/T过渡附近消散，导致形成斑驳的硅酸盐云层和晚期L矮星和早期T矮星的高振幅变化[49]。 云的中断使更深的云层可被用于观测；这些较深的层更温暖并含有FeH。这解释了FeH的重新出现和增强，以及早期到中期T矮星的蓝色近红外颜色[25]。晚期T矮星也应该有由铬、氯化钾和不同的 硫化物组成的云层。这些云层很薄，并且存在于硅酸盐云的上方[49]。一颗可变的晚T矮星是WISE 0458+6434（T8.5），在一个周期内变化了13%[50]。

磁场和极光

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在电波发射中探测到的第一颗T矮星是2MASS J1047+21（T6.5），它是用阿雷西博电波望远镜发现的[51]。从那时起，其它几颗具有无线电发射的T矮星被发现，包括行星质量天体SIMP J013656.5+093347（T2.5）[44]，以及在电波发射的说明下发现的T矮星BDR J1750+3809[52]。具有无线电发射的最冷T矮星是 WISEPA J062309.94-045624.6（T8）[53]。T矮星的电波发射类似于晚期L矮星，被认为是由极光产生的。此外H-α发射通常与L4-T8 矮星中的无线电发射有关，并被认为来自极光[54]。于 2000年发现的2Mass 1237+6526（T6.5）是一颗不寻常的强H-α发射T矮星[55]。理论上，H-α 发射、UV发射和无线电发射要么来自冷伴星（1-2.8 R🜨；<500 K）要么来自极光[56]。

联星

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晚期T矮星联星比L型联星少见。只有8±6%具有T5-Y0主系统的系统是联星，并且这些系统通常有几个天文单位（AU）的分离[57]。一颗著名的T矮星联星是波斯七（印地安座ε）[58]。这个联星由一颗T1和一颗T6矮星组成，它们彼此绕行，间隔为2.65 AU[59]。T矮星也存在三合星系统，2M0838+15是第一个被发现的完全分辨的T矮星三合星[60]。

相关条目

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参考资料

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