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Depression impairs self-management in diabetic patients, exacerbates insulin resistance, and elevates glycated hemoglobin (HbA1c) levels, thereby increasing diabetes risk. This study analyzed data from 30,386 participants in the National Health and Nutrition Examination Survey (NHANES), assessing depression severity using the 9-item Patient Health Questionnaire (PHQ-9) and evaluating diabetes status through clinical markers such as HbA1c, random blood glucose, and fasting blood glucose. Participants were stratified by depression severity and diabetes status to examine the relationship between depression and diabetes risk. We applied descriptive statistics, logistic regression models, subgroup analyses, and restricted cubic spline (RCS) modeling to explore this association. The results revealed that greater depression severity was significantly associated with increased diabetes incidence, elevated HbA1c, fasting glucose, and insulin levels. Multivariate regression analysis confirmed a consistent positive correlation between depression severity and diabetes risk. Subgroup analyses further identified significant relationships between depression and various demographic and behavioral factors, including gender, race, BMI, smoking status, and prediabetic conditions. Additionally, the RCS model demonstrated a clear increase in diabetes risk with rising PHQ-9 scores. In conclusion, our study demonstrates that the severity of depression is positively correlated with the risk of diabetes, and this association may be closely linked to various glycemic and lipid metabolic parameters.

Background The uric acid to high-density lipoprotein cholesterol ratio (UHR) has emerged as a novel metabolic marker and is proven to be associated with diabetes risk. However, there is still a lack of systematic research regarding its role in gender differences and underlying mechanisms. This study aims to assess the association of UHR with diabetes risk in the context of gender differences and to investigate its mediation effects through metabolic and inflammatory pathways. Methods This study utilized data from NHANES 2005–2010 and included 6,843 adult participants. Multivariate logistic regression was employed to assess the association between UHR and diabetes risk, and restricted cubic spline (RCS) along with correlation analysis was applied to explore its relationship with metabolic risk factors. Multiple mediation analysis was conducted to evaluate the mediating effects of homeostasis model assessment of insulin resistance (HOMA-IR), triglycerides (TG), and C-reactive protein (CRP) on the association between UHR and diabetes risk. Results In the overall population, UHR was significantly positively associated with diabetes risk, but gender-stratified analysis revealed a stronger predictive effect in women. In the unadjusted model, every unit increase in UHR was linked to an 18.6% increase in diabetes risk in women ( p  < 0.001). In the quartile analysis, women in the highest quartile showed an 8.49-fold increased risk of diabetes (OR = 8.494, 95% CI: 5.542–13.019, p  < 0.001), whereas no significant association was observed in men ( p  > 0.05). Mediation analysis revealed that HOMA-IR was the main mediator of the relationship between UHR and diabetes risk, with mediation effects of 64.55%, 118.38%, and 39.09% in the overall population, men, and women, respectively. Additionally, the mediation effect of TG was stronger in men (36.78%) and weaker in women (17.31%). The mediation effect of CRP was relatively minimal across all groups, accounting for 7.62% in men and 2.67% in women. Conclusion This study demonstrates that the association between UHR and diabetes risk exhibits gender differences, with higher diabetes risk observed in women, while men show stronger mediation effects in insulin resistance, lipid metabolism, and inflammatory response.

Type 2 diabetes mellitus (T2DM) and Major depressive disorder (MDD) act as risk factors for each other, and the comorbidity of both significantly increases the all-cause mortality rate. Therefore, studying the diagnosis and treatment of diabetes with depression (DD) is of great significance. In this study, we progressively identified hub genes associated with T2DM and depression through WGCNA analysis, PPI networks, and machine learning, and constructed ROC and nomogram to assess their diagnostic efficacy. Additionally, we validated these genes using qRT-PCR in the hippocampus of DD model mice. The results indicate that UBTD1, ANKRD9, CNN2, AKT1, and CAPZA2 are shared hub genes associated with diabetes and depression, with ANKRD9, CNN2 and UBTD1 demonstrating favorable diagnostic predictive efficacy. In the DD model, UBTD1 ( p  > 0.05) and ANKRD9 ( p  < 0.01) were downregulated, while CNN2 ( p  < 0.001), AKT1 ( p  < 0.05), and CAPZA2 ( p  < 0.01) were upregulated. We have discussed their mechanisms of action in the pathogenesis and therapy of DD, suggesting their therapeutic potential, and propose that these genes may serve as prospective diagnostic candidates for DD. In conclusion, this work offers new insights for future research on DD.

All stellar-mass black holes have hitherto been identified by X-rays emitted from gas that is accreting onto the black hole from a companion star. These systems are all binaries with a black-hole mass that is less than 30 times that of the Sun 1 – 4 . Theory predicts, however, that X-ray-emitting systems form a minority of the total population of star–black-hole binaries 5 , 6 . When the black hole is not accreting gas, it can be found through radial-velocity measurements of the motion of the companion star. Here we report radial-velocity measurements taken over two years of the Galactic B-type star, LB-1. We find that the motion of the B star and an accompanying Hα emission line require the presence of a dark companion with a mass of 68 − 13 + 11 solar masses, which can only be a black hole. The long orbital period of 78.9 days shows that this is a wide binary system. Gravitational-wave experiments have detected black holes of similar mass, but the formation of such massive ones in a high-metallicity environment would be extremely challenging within current stellar evolution theories. Radial-velocity measurements of a Galactic B-type star show a dark companion that seems to be a black hole of about 68 solar masses, in a widely spaced binary system.

Typically, neutron stars are discovered by observations at radio, X-ray or gamma-ray wavelengths. Unlike radio pulsar surveys and X-ray observations, optical time-domain surveys can unveil and characterize exciting but less explored non-accreting and/or non-beaming neutron stars in binaries. Here we report the discovery of such a neutron star candidate using the LAMOST spectroscopic survey. The candidate, designated LAMOST J112306.9 + 400736, is in a single-lined spectroscopic binary containing an optically visible M star. The star’s large radial velocity variation and ellipsoidal variations indicate a relatively massive unseen companion. Utilizing follow-up spectroscopy from the Palomar 200 in. telescope and high-precision photometry from the Transiting Exoplanet Survey Satellite, we measure a companion mass of 1.2 4 − 0.03 + 0.03 M ⊙ . Main-sequence stars with this mass are ruled out, leaving a neutron star or a massive white dwarf. Although a massive white dwarf cannot be excluded, the lack of UV excess radiation from the companion supports the neutron star hypothesis. Deep radio observations with the Five-hundred-meter Aperture Spherical radio Telescope (FAST) yielded no detections of either pulsed or persistent emission. J112306.9 + 400736 is not detected in numerous X-ray and gamma-ray surveys, suggesting that the neutron star candidate is not currently accreting and pulsing. Our work exemplifies the capability of discovering compact objects in non-accreting close binaries by synergizing optical time-domain spectroscopy and high-cadence photometry. A neutron star candidate in a close binary has been discovered using a radial velocity method and characterized with a variety of ground- and space-based telescopes. The system probably represents an underexplored population of non-accreting and/or non-beaming neutron stars.

Using the homogeneous X-ray catalog from ROSAT observations, we conducted a comprehensive investigation into stellar X-ray activity-rotation relations for both single and binary stars. Generally, the relation for single stars consists of two distinct regions: a weak decay region, indicating a continued dependence of the magnetic dynamo on stellar rotation rather than a saturation regime with constant activity, and a rapid decay region, where X-ray activity is strongly correlated with the Rossby number. Detailed analysis reveals more fine structures within the relation: in the extremely fast rotating regime, a decrease in X-ray activity was observed with increasing rotation rate, referred to as super-saturation, while in the extremely slow rotating region, the relation flattens, mainly due to the scattering of F stars. This scattering may result from intrinsic variability in stellar activities over one stellar cycle or the presence of different dynamo mechanisms. Binaries exhibit a similar relation to that of single stars while the limited sample size prevented the identification of fine structures in the relation for binaries. We calculated the mass loss rates of planetary atmosphere triggered by X-ray emissions from host stars. Our findings indicate that for an Earth-like planet within the stellar habitable zone, it would easily lose its entire primordial H/He envelope (equating to about 1% of the planetary mass).

The magnetic dynamo mechanism of giant stars remains an open question, which can be explored by investigating their activity-rotation relations with multiple proxies. By using the data from the LAMOST and \\emph{GALEX} surveys, we carried out a comprehensive study of activity-rotation relations of evolved stars based on \\cahk lines, \\(\\rm{H\\alpha}\\) lines and near ultraviolet (NUV) emissions. Our results show that evolved stars and dwarfs obey a similar power-law in the unsaturated region of the activity-rotation relation, indicating a common dynamo mechanism in both giant and dwarfs. There is no clear difference in the activity levels between red giant branch stars and red clump stars, nor between single giants and those in binaries. Additionally, our results show that the NUV activity levels of giants are comparable to those of G- and K-type dwarfs and are higher than those of M dwarfs.

We report the discovery of a close binary J0606+2132 (Gaia DR3 3423365496448406272) with \\(P_{\\rm obs}=2.77\\) days containing a possible massive white dwarf or a neutron star using the LAMOST spectroscopic data. By a joint fitting of the radial velocity from LAMOST and the light curve from TESS, we derived a circular Keplerian orbit with an inclination of \\(i=\\)81.31$^{\\circ}$$^{+6.26^{\\circ}}_{-7.85^{\\circ}}\\(, which is consistent with that derived from \\)v{\\rm sin}I\\(. Together with the mass of the visible star, we derived the mass of the invisible object to be 1.34\\)^{+0.35}_{-0.40} M_{\\odot}$. Spectral disentangling with the LAMOST medium-resolution spectra shows no absorption feature from an additional component, suggesting the presence of a compact object. No X-ray or radio pulsed signal is detected from ROSAT and FAST archive observations. J0606+2132 could evolve into either a Type Ia supernova or a neutron star through accretion-induced collapse if it is a white dwarf, or into an intermediate-mass X-ray binary if it is a neutron star.

The Doppler beaming effect, induced by the reflex motion of stars, introduces flux modulations and serves as an efficient method to photometrically determine mass functions for a large number of close binary systems, particularly those involving compact objects. In order to convert observed beaming-flux variations into a radial-velocity curve, precise determination of the beaming factor is essential. Previously, this factor was calculated as a constant, assuming a power-law profile for stellar spectra. In this study, we present a novel approach to directly compute this factor. Our new method not only simplifies the computation, especially for blue bands and cool stars, but also enables us to evaluate whether the relationship between beaming flux and radial velocity can be accurately described as linear. We develop a python code and compute a comprehensive beaming-factor table for commonly used filter systems covering main-sequence, subgiant, and giant stars, as well as hot subdwarf and white dwarf stars. Both the code and our table are archived and publicly available at http://doi.org/10.5281/zenodo.13049419.