Understanding High-Energy (UV and X-ray) Emission from AGB Stars—Episodic Accretion in Binary Systems

: X-ray surveys of UV-emitting AGB stars show that ∼ 40% of objects with FUV emission and GALEX FUV/NUV ﬂux ratio R fuv / nuv > ∼ 0.2 (fuvAGB stars) have variable X-ray emission characterized by very high temperatures (Tx ∼ 35–160 MK) and luminosities (Lx ∼ 0.002–0.2 L (cid:12) ), indicating the presence of accretion associated with a close binary companion. However, the UV-emitting AGB star population is dominated by objects with R fuv / nuv (cid:46) 0.06 (nuvAGB stars), and we do not know whether the UV emission from these is intrinsic to the AGB star or extrinsic (i.e., due to binarity). In order to help distinguish between intrinsic and extrinsic models of the puzzling high-energy emission of cool AGB stars, we report results from two studies—(i) XMM-Newton X-observations of two nuvAGB stars, and (ii) simple chromosphere modeling. In study (i), we detect the one which has the lower FUV/NUV ratio, with a total Lx = 0.00027 L (cid:12) , and a spectrum best ﬁtted with a dominant component at Tx ∼ 10MK, most likely coronal emission from a main-sequence companion. Therefore, a signiﬁcant fraction of nuvAGB stars may also be binaries with active, but weak accretion. Study (ii) shows that chromospheres with temperatures of ∼ 10,000K can produce R fuv / nuv (cid:46) 0.06; higher ratios require hotter gas, implying active accretion.


Introduction
Stars in the 1-8 M range expel half or more of their masses at rates up to ∼10 −4 M yr −1 (e.g., Decin 2021 [1], Olofsson 2008 [2]), as they evolve from the asymptotic giant branch (AGB) to the preplanetary nebula (PPN) and planetary nebula (PN) evolutionary phases. This mass loss dramatically alters the course of stellar evolution, enriches the interstellar medium (ISM) with nucleosynthetically enriched material and thus plays a key role in the chemical evolution of galaxies. AGB stars also eject copious quantities of dust grains into the ISM, which are crucial ingredients for the birth of new Sun-like stars and solar systems. Young PNe (YPNe) represent the bright end-stages of these stars and provide valuable diagnostics on their demise. However, YPNe formation and the phase of extreme mass loss at the end of the AGB phase is very poorly understood-although the mass ejection in the latter is generally spherical, producing extended circumstellar envelopes (CSEs) expanding at speeds of 10-20 km s −1 , all observed PPNe and most YPNe are observed to have bipolar, multipolar or elliptical shapes (e.g., Sahai and Trauger 1998 [3] [ST98], Sahai et al. 2007 [4], Sahai et al. 2011 [5] [SMV11]). Collimated high-speed outflows ( (50-100) km s −1 ) are ubiquitous during the PPN phase (Bujarrabal et al. 2001 [6]).
Morphologically unbiased HST imaging surveys have observationally bracketed the evolutionary phases that cover the transition from the spherical to aspherical morphology. These surveys imaged (1) nascent PPNe (IRAS 25-12 µm flux ratio 1 < F25/F12 < 1.4, to select for objects lacking hot dust, as an indicator that dense AGB mass loss is decreasing) (Sahai et al. 2006 [7]), (2) PPNe (F25/F12 > 1.4, to select for objects lacking warm dust, as an indicator that dense AGB mass loss has stopped recently) (Sahai et al. 2007 [4]), and (3) YPNe (i.e., compact, with size 10 , and the flux ratio [OIII]/Hα 1) (ST98, SMV11). The PPN and YPN surveys led to a systematic characterization scheme for the observed morphologies with four primary classes (B: bipolar, M: multipolar, E: elongated, and I: irregular) (e.g., Figure 1a-h). No round PPN was found. Nascent PPNe look morphologically different from PPNe and YPNe, typically showing asymmetric elongated structures (Figure 1j,k). Such structures could result from either (a) an aspherical density distribution, and/or (b) aspherical illumination. Case (b) would require the presence of relatively low-density channels close to the central star, which allow the starlight to escape preferentially along specific directions, and illuminate more distant regions of the circumstellar medium in an aspherical manner. In either case, the mechanism for creating the large-scale density inhomogeneities is likely to be a high-velocity outflow that has just begin to sculpt the innermost regions of the AGB mass-loss envelope.  Figure 1. YPNe, PPNe, and nascent PPNe images from HST-(a-f) Hα (or [NII]) images of PNe belonging to 6 primary classes in the Sahai, Morris, and Villar (2011) [5] classification system, which consists of 7 primary classes based on the overall nebular shape, and several categories of secondary characteristics related to specific properties of the lobes, waist, and haloes, and the presence of point-symmetry; (g,h) 0.6 µm images of PPNe belonging to 2 primary classes; and (j,k) 0.6 µm images of nascent PPNe. (a) PNG 014.3 − 05.5 (4. 0 × 4. 0), (b) PNG 027.6 − 09.6 (11. 4 × 11. 4), (c So what is the underlying cause (or causes) of this dramatic AGB-to-PN transition? Binary interactions, directly or indirectly, are now widely believed to be the culprit. These include common-envelope ejection (Ivanova et al. 2013 [8]) or grazing envelope evolution (Soker 2015 [9]) and/or accretion disk and torus formation, or indirectly via increased rotation and the generation of strong magnetic fields (e.g., Blackman et al. 2001 [10]). Binaries provide a source of angular momentum and free energy to form accretion disks and such disks can in turn amplify magnetic fields that can transport angular momentum on large scales (Blackman and Lucchini 2014 [11]). The latter process can result in high-speed, collimated jet-like outflows that sculpt the surrounding spherical circumstellar envelopes from the inside out during the late AGB or early PPN phase, producing bipolar and multipolar shapes (ST98). Yet most of our current understanding of this late evolutionary stage is based on single-star models! One reason for this is the lack of observational evidence for close binary companions in AGB stars. AGB stars are very luminous and variable, invalidating standard techniques for binary detection (e.g., radial-velocity and photometric variations due to a companion star and direct imaging.) Interestingly, the long secondary periods found for many RGB and AGB stars provides possible new evidence for the presence of close companions (Wood et al. 1999 [12], Soszyński et al. 2021 [13]). Sahai et al. (2008) [14] were the first to show that UV observations can be used to search for binarity and associated accretion activity in AGB stars because most of these are relatively cool (T e f f < ∼ 3000 K) objects (spectral types ∼M6 or later), whereas any stellar companions and/or accretion disks around them are likely significantly hotter (T e f f > ∼ 6000 K), so that favorable secondary-to-primary flux contrast ratios ( > ∼ 10) are reached in the GALEX FUV (1344-1786 Å) and NUV (1771-2831 Å) bands for a source (companion or disk) with T e f f > ∼ 6000 K and luminosity L > ∼ 1 L . From an application of this technique to a volumelimited sample (<0.5 kpc) of 58 AGB stars, Ortiz, and Guerrero (2016) [15] conclude that the detection of FUV emission or an observed-to-predicted ratio for NUV emission of Q NUV > 20 are criteria for binarity.

UV Emission
UV spectroscopy can provide an unambiguous probe of accretion-related activity because the latter is expected to produce UV lines with large widths and large Doppler shifts. An HST/STIS spectroscopic study of the prototype fuvAGB star, Y Gem, shows the presence of high-velocity infalling and outflowing material as well as flickering, and thus directly supports the binary/accretion hypothesis (see Figure 2 and Sahai et al. 2018 [16]). The UV spectrum of Y Gem shows lines from species such as Si IV and C IV (Figure 2a), with broad emission and absorption features (FWHM∼300-700 km s −1 ) that are, respectively, red-and blue-shifted by velocities of ∼500 km s −1 from the systemic velocity. The UV continuum reveals strong flickering on time scales of 20 s (Figure 2c), characteristic of an active accretion disk with an accretion hot spot of size 0.1 au. A two-blackbody model that fits the G140L and G230L spectra shows significant variations in the luminosity (Figure 2d), but not in the temperature. Since neither of these two blackbodies fit the properties of a viable stellar companion (WD or MS) to the primary, it is likely that both the hot and cool UV components arise in a hot accretion disk, which results from the gravitational capture of material from the primary star by a low-mass main-sequence companion. A simple geometric model can then qualitatively explain the Doppler shifts of the absorption and emission features observed in the UV spectra: the accretion disk captures part of the material in an outflow or Roche-lobe overflow from the primary AGB star, via two possible infall streams-these produce red-shifted emission features. Assuming that the total luminosity of the blackbody components, L acc = 13 L , results from accretion, the mass accretion rate resulting from the infall is L acc R c /G M c 5 × 10 −7 M yr −1 , where R c = 0.44 R and M c = 0.35 M are the radius and mass of the companion (Sahai et al. 2015 [17]), and G is the gravitational constant. The accretion disk powers a fast outflow that absorbs UV photons from the disk, producing blue-shifted absorption features.

X-ray Emission
The detection of X-rays towards AGB stars provides strong supporting evidence for accretion activity. An AGB star is unlikely to be a source of X-ray emission, since it would require rather strong magnetic fields to confine the hot plasma, and sensitive searches for X-rays in two AGB stars with strong magnetic fields have been unsuccessful (Kastner and Soker 2004 [18]), but it cannot be ruled out. Alternatively, a secondary component would provide the X-ray flux from AGB stars, either originating in an accretion disk around the secondary, or in the corona of an MS companion.
X-ray-emitting AGB stars have been found both in targeted X-ray searches in selected samples of AGB stars with high values (>0.17) of R f uv/nuv (Sahai et al. 2015 [9]) as well as serendipitous detections in an archival survey (Ortiz and Guerrero 2021 [19]). The X-ray emission is variable, both on long ( Figure 3) and short (Figure 4) time scales and may be related to variations in the accretion-flow and/or the circumstellar absorbing column. The short-term variability is similar to the flickering observed in the STIS study of Y Gem (see above). The Astrophysica Plasma Emission Code (APEC; Smith et al. 2001 [20]) was used to fit the X-ray spectra of five sources with the highest S/N X-ray spectra (two of these are shown in Figure 3). We find that the observed X-ray luminosity (Lx) and temperature (Tx) lie in the range Lx∼(0.002-0.2) L and Tx∼(3.5-16) × 10 7 K. The high X-ray temperatures argue against the emission arising in stellar coronae, and the high X-ray luminosities specifically argue against emission originating in the coronae of main-sequence companions for the high R f uv/nuv AGB stars observed by Sahai et al. (2015) [17].
There is strong evidence that the X-ray emission is associated with the far-UV flux, and both result from accretion activity. We find that R f uv/nuv is a better indicator of X-ray emission than the FUV (or NUV) flux alone. For example, when AGB stars are classified into fuvAGB (i.e., those with the GALEX FUV/NUV ratio R f uv/nuv > 0.15) and nuvAGB (R f uv/nuv < 0.06), we observe that X-ray emission has been detected only in fuvAGB stars with R f uv/nuv > 0.17) (including two ROSAT detections reported by Ramstedt et al. 2012 [21]) (see Figure 4b in Sahai et al. 2015 [17]).
The far-UV and near-UV emission might have different origins. For instance, Montez et al. (2017) [22] found that the GALEX near-UV magnitude follows the stellar pulsation (i.e., it is intrinsic, likely dominated by chromospheric emission from the AGB star), whereas the far-UV does not show this correlation, and its more likely to be extrinsic, likely dominated by emission from an accretion disk.

Models of Chromospheric Emission
We now investigate the question of what mechanism best explains the high-energy emission-accretion activity in a binary or chromospheric emission. The studies above strongly indicate that when R f uv/nuv is high, the origin of the high-energy emission is accretion activity. However, when it is low, either or both of these mechanisms may be responsible. Sahai et al. 2015 [17] show that if the X-ray luminosity Lx > 0.001 L , as found for their sample of fuvAGB stars, it is too high to arise in an MS companion's corona. Similarly, the observed FUV emission in AGB stars ( 10 µJy, see below) is too high to arise in an MS companion's chromosphere. The FUV flux of an MS Sun-like companion with a luminosity of, e.g., ∼1 L , at the typical distances of AGB stars, >100 pc, is <0.1-0.01 µJy, taking (FUV/Fbol)∼10 −4 -10 −5 (see Figure 5 panels c,d of Viswanath et al. 2020 [23]; FUV is the UV flux integrated over the GALEX FUV bandpass, and Fbol is the bolometric flux).
We address this question by first considering the UV properties of a large sample of ∼3500 AGB stars with spectral types M4 or later. This sample was constructed using the Hipparcos database as follows. First, we selected all stars with spectral type M (field H69 of the main Hipparcos catalog). From this list, we chose only those which simultaneously satisfied the color conditions: V − I > B − V, B − V > 1, and V − I > 1.5, allowing us to remove misclassified stars which were of intrinsically earlier spectral types. Finally, main-sequence M stars were removed by rejecting stars with parallaxes π >20 mas: since the limiting V magnitude of Hipparcos is ∼12.4, any main-sequence M star (with a typical absolute magnitude of M V ∼9) would not be detectable at distances 50 pc. We found that >20% were detected in one or both of the GALEX FUV and NUV bands, and about >9% were detected in both. These percentages are lower limits because most of the GALEX data come from the All-Sky Imaging Survey (AIS), which had relatively short exposure times, ∼(1 − f ew) × 100 s.
The mean FUV ( f FUV ) and NUV ( f NUV ) for all stars in the database which were detected in both these bands (316 objects) show a linear relationship-we find that f FUV = R FUV/NUV × f NUV provides a good fit to the bulk of the data, with R FUV/NUV = 0.061 ± 0.0015. Outliers, defined as data where the observed f FUV value was ≥ 5σ away from the model fit, were removed iteratively until the slope and number of outliers converged (in six iterations), resulting in the removal of 17 outliers. Restricting our dataset to objects where the SNR for both the mean FUV and NUV was ≥5 (a total of 184 objects: Figure 5) did not affect the results significantly-we found R FUV/NUV = 0.060 ± 0.0022 after five iterations, with 14 outliers. We show below that models of chromospheric emission can explain R f uv/nuv 0.06: thus the outliers for which R f uv/nuv is significantly above 0.06 are objects where accretion activity is likely responsible for the UV emission, and the outliers for which R f uv/nuv is significantly below 0.06 are objects where chromospheres are weak or absent. We made a large grid of simple chromospheric models (∼50,000) using the CLOUDY code (Ferland et al. 2017 [24]) to compute the UV emission from a collisionally ionized plasma with temperature T chrom and density nH contained within a layer of gas of thickness ∆ R surrounding the AGB star. We show the observed R f uv/nuv versus the FUV-to-K band flux ratio for our sample of UV-emitting AGB stars, R FUV/K , together with model values, in Figure 6-the latter is a good proxy for the fractional FUV luminosity, since the K-band flux is expected to result almost entirely from the emission from the AGB photosphere, excluding the effect of the presence of dust that may be present in a stellar wind.
We found that our chromosphere models can produce R f uv/nuv ∼0.06 for temperatures in the range 9000 ≤ T chrom (K) ≤ 11,000. Higher values of R f uv/nuv require higher temperatures, e.g., for R f uv/nuv ∼0.1, it requires 11,000 ≤ T chrom (K) ≤ 15,000. The allowed values of the parameters nH and ∆ R are not independent, because the total emission from a collisionally excited plasma (as assumed for the CLOUDY models) is expected to be proportional to the square of the density and the total volume of emitting material. We found that for 0.2 × 10 −6 (FUV/K) 0.3 × 10 −6 , where most of the AGB stars are located (Figure 6), the typical values of nH and ∆ R were 10 8.5 cm −3 and 0.5 au, respectively, for a typical AGB star of radius 1.5 au. We compared our model results to the detailed chromospheric models for the M6 AGB star, g Her by Luttermoser et al. (1994) [25], based on fitting near-UV lines from the IUE data, with the greatest weight given to the Mg II h and k doublet (∼2800 Å), followed by Mg I (λ 2852 Å) and the CII] UV0.01 multiplet (∼2325 Å). The temperature distribution of their best-fit model, T10, ranged from 11,270 K to 3200 K. The model chromospheric layer extended from the photosphere to a height of ∼1.7 au, with temperatures in the range ∼9000-11,270 K at heights 0.45 au. Our simple models thus appear to be a reasonable approximation to a more detailed model of the chromosphere for the purpose of investigating the dependence of R f uv/nuv on T chrom .

Search for X-ray Emission from nuvAGB Stars
We also carried out a small survey of bright nuvAGB stars with XMM-Newton, i.e., stars with R f uv/nuv < 0.08. Out of the seven targets proposed, two were observed, TW Hor and Oct. We found the somewhat surprising result that TW Hor, which has R f uv/nuv = 0.044, was detected, whereas Oct, which has a higher value of R f uv/nuv (0.057), was not. An APEC model fit to the X-ray spectra of TW Hor showed that Tx∼10 7 K and Lx∼0.0003 L , most likely thermal emission from coronal gas (Figure 7a).   Since AGB stars are unlikely to have sufficiently strong magnetic fields to confine the hot plasma, it is likely that the coronal gas in nuvAGB stars is associated with a mainsequence companion. These results suggest that a significant fraction of AGB stars with low FUV/NUV ratios, such as those with high FUV/NUV ratios, are also binaries. The soft X-ray component in such stars may be coronal emission from a main-sequence companion; if this hypothesis is correct, then we should expect to find examples of objects which show X-ray emission from both the companion's corona as well as accretion activity. RR UMi (sp. type M5), with R f uv/nuv = 0.29, is a plausible example. It shows X-ray emission that is best-fitted with a two-component APEC model, with the dominant component being soft, with Tx∼6.6 × 10 6 K, resulting from the companion's corona and a secondary, harder component, with Tx∼10 8 K, due to accretion activity (Figure 7b).

Summary and Conclusions
Binarity interactions and accretion are now widely believed to play a major role in the death throes of most stars in the Universe that evolve in a Hubble time. UV and X-ray studies of AGB stars have now begun to provide robust observational evidence for binarity and associated accretion activity. Our main results are: • A survey of ∼3500 galactic AGB stars (sp.types M4-M10) reveals that a significant fraction of this population show UV emission ( 9% NUV and FUV, and 20% NUV). • The UV emission is variable, indicative of variable accretion activity, presumably due to a binary companion; this inference is supported by a detailed spectroscopic study of the star Y Gem. • For stars with R f uv/nuv 0.06, simple chromosphere models cannot produce the observed UV emission, and accretion activity in a binary is the most likely mechanism for UV emission (supported by X-ray studies). • For stars with R f uv/nuv 0.06, simple chromosphere models can produce the observed UV emission; however the, X-ray detection of one out of two such stars suggests that some fraction of these may also be in binary systems but with low accretion rates.

Data Availability Statement:
All the data reported in this study, except the X-ray data on TW Hor and Oct, are available from the XMM-Newton, Chandra X-ray Observatory, and GALEX archives.