The Symbiotic X-Ray Binary IGR J16194-2810: A Window on the Future Evolution of Wide Neutron Star Binaries From Gaia

IF 3.3 3区 物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS
Pranav Nagarajan, Kareem El-Badry, Casey Lam and Henrique Reggiani
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Abstract

We present optical follow-up of IGR J16194-2810, a hard X-ray source discovered by the INTEGRAL mission. The optical counterpart is a ∼500 L⊙ red giant at a distance of 2.1 kpc. We measured 17 radial velocities (RVs) of the giant over a period of 271 days. Fitting these RVs with a Keplerian model, we find an orbital period of Porb = 192.73 ± 0.01 days and a companion mass function f(M2) = 0.365 ± 0.003 M⊙. We detect ellipsoidal variability with the same period in optical light curves from the ASAS-SN survey. Joint fitting of the RVs, light curves, and the broadband spectral energy distribution allows us to robustly constrain the masses of both components. We find a giant mass of and a companion mass of , implying that the companion is a neutron star (NS). We recover a 4.06 hr period in the system’s TESS light curve, which we tentatively associate with the NS spin period. The giant does not yet fill its Roche lobe, suggesting that current mass transfer is primarily via winds. Modules for Experiments in Stellar Astrophysics evolutionary models predict that the giant will overflow its Roche lobe in 5–10 Myr, eventually forming a recycled pulsar + white dwarf binary with a ∼900 days period. IGR J16194-2810 provides a window on the future evolution of wide NS + main sequence binaries recently discovered via Gaia astrometry. As with those systems, the binary’s formation history is uncertain. Before the formation of the NS, it likely survived a common envelope episode with a donor-to-accretor mass ratio ≳10 and emerged in a wide orbit. The NS likely formed with a weak kick (vkick ≲ 50 km s−1), as stronger kicks would have disrupted the orbit.
共生X射线双星IGR J16194-2810:从盖亚观测宽中子星双星未来演化的窗口
我们将对INTEGRAL任务发现的硬X射线源IGR J16194-2810进行光学跟踪。它的光学对应体是一颗距离 2.1 kpc 的 ∼500 L⊙红巨星。我们测量了这颗红巨星在 271 天内的 17 个径向速度(RV)。用开普勒模型拟合这些径向速度,我们发现其轨道周期为 Porb = 192.73 ± 0.01 天,伴星质量函数 f(M2) = 0.365 ± 0.003 M⊙。我们从ASAS-SN巡天的光学光变曲线中探测到了具有相同周期的椭圆变率。联合拟合 RVs、光曲线和宽带光谱能量分布,使我们能够有力地约束这两个成分的质量。我们发现巨星质量为 ,伴星质量为 ,这意味着伴星是一颗中子星(NS)。我们在该系统的 TESS 光曲线中发现了一个 4.06 小时的周期,我们暂时将其与 NS 的自旋周期联系起来。这颗巨星还没有填满它的罗切叶,这表明目前的质量转移主要是通过风进行的。恒星天体物理学实验模块演化模型预测,这颗巨星将在5-10 Myr后溢出其罗氏叶,最终形成一个周期为900天的循环脉冲星+白矮星双星。IGR J16194-2810为观察最近通过盖亚天体测量发现的宽NS+主序双星的未来演化提供了一个窗口。与这些系统一样,该双星的形成历史也不确定。在NS形成之前,它很可能经历了一次捐献者与激发者质量比≳10的普通包络事件,并出现在一个宽轨道上。NS很可能是在一个较弱的踢脚(vkick ≲ 50 km s-1)作用下形成的,因为较强的踢脚会扰乱轨道。
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来源期刊
Publications of the Astronomical Society of the Pacific
Publications of the Astronomical Society of the Pacific 地学天文-天文与天体物理
CiteScore
6.70
自引率
5.70%
发文量
103
审稿时长
4-8 weeks
期刊介绍: The Publications of the Astronomical Society of the Pacific (PASP), the technical journal of the Astronomical Society of the Pacific (ASP), has been published regularly since 1889, and is an integral part of the ASP''s mission to advance the science of astronomy and disseminate astronomical information. The journal provides an outlet for astronomical results of a scientific nature and serves to keep readers in touch with current astronomical research. It contains refereed research and instrumentation articles, invited and contributed reviews, tutorials, and dissertation summaries.
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