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The emission from the accreting black holes (BHs) in low-mass X-ray binaries(LMXBs) covers a broad energy band from radio to X-rays. Studying thecorrelations between emission in different energy bands during outbursts canprovide valuable information about the accretion process. We analyse thesimultaneous optical, ultraviolet (UV) and X-ray data of the BH-LMXB SwiftJ1753.5-0127 during its $\sim$ 12-year long outburst with the {\it Neil GehrelsSwift Observatory}. We find that the UV/optical and X-ray emission are stronglycorrelated during the hard states of the outburst. We fit the relation with apower-law function $F_{UV/optical} \propto F_{X}^{\beta}$ and find that thepower-law index $\beta$ increases from $\sim$ 0.24 to $\sim$ 0.33 as theUV/optical wavelength decreases from $\sim$ 5400 \r{A} (V) to $\sim$ 2030 \r{A}(UVW2). We explore the possible reasons for this and suggest that in SwiftJ1753.5-0127 the UV/optical emission is dominated by a viscously heatedaccretion disc at large radii. We find that the data that deviate from thecorrelation correspond to the low-intensity peaks appeared in the X-ray bandduring the outburst, and suggest that these deviations are driven by theemission from the inner part of the accretion disc.

The origin of UV/optical emission in the black hole low-mass X-ray binary Swift J1753.5-0127